[
{
"id": "authors:5h27s-bx682",
"collection": "authors",
"collection_id": "5h27s-bx682",
"cite_using_url": "https://authors.library.caltech.edu/records/5h27s-bx682",
"type": "article",
"title": "LIGO/Virgo/KAGRA Neutron Star Merger Candidate S250206dm: Zwicky Transient Facility Observations",
"author": [
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumada-Tom\u00e1s"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "Gupta",
"given_name": "Vaidehi",
"orcid": "0000-0002-7672-0480"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Jegou du Laz",
"given_name": "Theophile",
"orcid": "0009-0003-6181-4526",
"clpid": "Jegou-Du-Laz-Theophile"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Banerjee",
"given_name": "Smaranika",
"orcid": "0000-0001-6595-2238"
},
{
"family_name": "Bochenek",
"given_name": "Aleksandra",
"orcid": "0009-0008-2714-2507"
},
{
"family_name": "Hinds",
"given_name": "K-Ryan",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Hu",
"given_name": "Lei",
"orcid": "0000-0001-7201-1938"
},
{
"family_name": "Palmese",
"given_name": "Antonella",
"orcid": "0000-0002-6011-0530"
},
{
"family_name": "Perley",
"given_name": "Daniel",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Pletskova",
"given_name": "Natalya",
"orcid": "0009-0008-8062-445X"
},
{
"family_name": "Salgundi",
"given_name": "Anirudh",
"orcid": "0000-0003-3173-4691"
},
{
"family_name": "Singh",
"given_name": "Avinash",
"orcid": "0000-0003-2091-622X"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Swain",
"given_name": "Vishwajeet",
"orcid": "0000-0002-7942-8477"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Copperwheat",
"given_name": "Chris",
"orcid": "0000-0001-7983-8698"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597"
},
{
"family_name": "Sravan",
"given_name": "Niharika"
},
{
"family_name": "Busmann",
"given_name": "Malte",
"orcid": "0009-0001-0574-2332"
},
{
"family_name": "Gassert",
"given_name": "Julius",
"orcid": "0009-0008-2754-1946"
},
{
"family_name": "Gruen",
"given_name": "Daniel",
"orcid": "0000-0003-3270-7644"
},
{
"family_name": "Sommer",
"given_name": "Julian",
"orcid": "0000-0002-1154-8317"
},
{
"family_name": "Zhang",
"given_name": "Yajie",
"orcid": "0000-0003-2976-8198"
},
{
"family_name": "Amsellem",
"given_name": "Ariel",
"orcid": "0000-0003-3433-2698"
},
{
"family_name": "Cabrera",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-1270-7666"
},
{
"family_name": "Hall",
"given_name": "Xander J.",
"orcid": "0000-0002-9364-5419"
},
{
"family_name": "Kunnumkai",
"given_name": "Keerthi",
"orcid": "0009-0000-4830-1484"
},
{
"family_name": "O'Connor",
"given_name": "Brendan",
"orcid": "0000-0002-9700-0036"
},
{
"family_name": "Barna",
"given_name": "Tyler",
"orcid": "0000-0002-4843-345X"
},
{
"family_name": "Fontinele Nunes",
"given_name": "Felipe",
"orcid": "0000-0001-7129-1325"
},
{
"family_name": "Toivonen",
"given_name": "Andrew",
"orcid": "0009-0008-9546-2035"
},
{
"family_name": "Sasli",
"given_name": "Argyro",
"orcid": "0000-0001-7357-0889"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank"
},
{
"family_name": "Chen",
"given_name": "Tracy X.",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-X"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Le Calloch",
"given_name": "Antoine",
"orcid": "0009-0009-7000-8343"
},
{
"family_name": "Anupama",
"given_name": "G. C.",
"orcid": "0000-0003-3533-7183"
},
{
"family_name": "Barway",
"given_name": "Sudhanshu",
"orcid": "0000-0002-3927-5402"
}
],
"abstract": "We present the searches conducted with the Zwicky Transient Facility (ZTF) in response to S250206dm, a bona fide event with an online false alarm rate of one in 25 yr, detected by the International Gravitational Wave Network. Although the event is significant, the nature of the compact objects involved remains unclear, with at least one likely neutron star. ZTF covered 68% of the last refined Bilby localization region, though we did not identify any likely optical counterpart. We describe the ZTF strategy, potential candidates, and the observations that helped rule out candidates, including sources circulated by other collaborations. Similar to Ahumada et al., we perform a frequentist analysis, using simsurvey , as well as Bayesian analysis, using nimbus , to quantify the efficiency of our searches. We find that, given the nominal up-to-date distance to this event of 373 ± 104 Mpc, our efficiencies are above 10% for KNe brighter than −17.5 absolute magnitude. Assuming the optical counterpart known as kilonova (KN) lies within the ZTF footprint, our limits constrain the brightest end of the KN parameter space. Through dedicated radiative transfer simulations of KNe from binary neutron star (BNS) and black hole–neutron star mergers, we exclude parts of the BNS KN parameter space. Up to 35% of the models with high wind ejecta mass (Mwind ≈ 0.13M\u2299) are ruled out when viewed face-on (\\(\\mathrm{cos}\\theta_{\\mathrm{obs}}=1.0\\)). Finally, we present a joint analysis using the combined coverage from ZTF and the Gravitational Wave Multimessenger Dark Energy Camera Survey. The joint observations cover 73% of the Bilby localization region, and the combined efficiency has a stronger impact on rising and slowly fading models, allowing us to rule out 55% of the high-mass KN models viewed face-on.
",
"doi": "10.1088/1538-3873/ae4539",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2026-03-01",
"series_number": "3",
"volume": "138",
"issue": "3",
"pages": "034101"
},
{
"id": "authors:rtznc-m2q24",
"collection": "authors",
"collection_id": "rtznc-m2q24",
"cite_using_url": "https://authors.library.caltech.edu/records/rtznc-m2q24",
"type": "article",
"title": "Efficacy of galaxy catalogues for following up gravitational wave events",
"author": [
{
"family_name": "Roychowdhury",
"given_name": "Tamojeet",
"orcid": "0009-0003-9906-2745"
},
{
"family_name": "Choudhary",
"given_name": "Harsh"
},
{
"family_name": "Bhalerao",
"given_name": "Varun"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kumar",
"given_name": "Harsh"
},
{
"family_name": "More",
"given_name": "Surhud"
},
{
"family_name": "Waratkar",
"given_name": "Gaurav"
}
],
"abstract": "The detection of gravitational waves (GW) by the LIGO-Virgo-KAGRA (LVK) network has opened up a new era in astrophysics. The identification of the electromagnetic counterparts of GW sources is crucial for multi-messenger astronomy, one way of which is to use galaxy catalogues to guide optical follow-up observations. In this paper, we test the utility of a galaxy-targeted approach with mass prioritised galaxy ranking for the ongoing LIGO O4 run. We have used the simulated results for the expected LIGO O4 events and the NED-LVS galaxy catalogue, and based our study on small field of view telescopes, specifically the GROWTH-India Telescope (GIT). With the increase in sensitivity of LIGO/Virgo in the ongoing observing run O4, the expected number of total detections have gone up, but most of these are also now poorly localised. We show that a larger volume covered in the same field-of-view (FoV) on the sky results in a large increase in the total number of galaxies in each FoV. A significant top-heaviness is observed in the mass-ranked list of galaxies, which still numbers a few thousand in most cases. At larger distances, such high numbers of deep follow-up observations are infeasible in most cases, rendering galaxy catalogues useful in limited cases. However, these are still useful at lower distances where LVK detectors are currently sensitive and where galaxy completeness is higher. We also explore the effect of mass-filling to account for galaxy catalogue incompleteness at large distances. If mass-filled probabilities are considered as the metric for ranking and coverage, we find that the conventional 2D probability search performs better than a 3D galaxy catalogue (without mass-filling) based search at distances larger than 300 Mpc (up to which NED-LVS is ~70% complete), and using 3D mass times probability in each tile performs better for nearby events.
",
"doi": "10.1007/s12036-025-10097-1",
"issn": "0973-7758",
"publisher": "Springer Science and Business Media LLC",
"publication": "Journal of Astrophysics and Astronomy",
"publication_date": "2025-12",
"series_number": "2",
"volume": "46",
"issue": "2",
"pages": "68"
},
{
"id": "authors:fqkbk-n3j73",
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"collection_id": "fqkbk-n3j73",
"cite_using_url": "https://authors.library.caltech.edu/records/fqkbk-n3j73",
"type": "article",
"title": "Low-luminosity Type IIP Supernovae from the Zwicky Transient Facility Census of the Local Universe. I. Luminosity Function, Volumetric Rate",
"author": [
{
"family_name": "Das",
"given_name": "Kaustav K.",
"orcid": "0000-0001-8372-997X",
"clpid": "Das-Kaustav-K"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331"
},
{
"family_name": "Sit",
"given_name": "Tawny",
"orcid": "0000-0001-8208-9755"
},
{
"family_name": "Adams",
"given_name": "Scott",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515"
},
{
"family_name": "Ahumuda",
"given_name": "Tomas",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumuda-Tom\u00e1s"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Brennan",
"given_name": "Se\u00e1n",
"orcid": "0000-0003-1325-6235"
},
{
"family_name": "Brink",
"given_name": "Thomas"
},
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0002-0786-7307"
},
{
"family_name": "Chen",
"given_name": "Ping",
"orcid": "0000-0003-0853-6427"
},
{
"family_name": "Chu",
"given_name": "Matthew R."
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Covarrubias",
"given_name": "Sofia",
"orcid": "0000-0003-1858-561X",
"clpid": "Covarrubias-Sofia"
},
{
"family_name": "Dahiwale",
"given_name": "Aishwarya",
"clpid": "Dahiwale-Aishwarya"
},
{
"family_name": "Earley",
"given_name": "Nicholas",
"orcid": "0000-0001-6627-9903",
"clpid": "Earley-Nicholas"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Gangopadhyay",
"given_name": "Anjasha",
"orcid": "0000-0002-3884-5637"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Hinds",
"given_name": "K-Ryan",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Kong",
"given_name": "Yihan"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Jegou du Laz",
"given_name": "Theophile",
"orcid": "0009-0003-6181-4526",
"clpid": "Jegou-Du-Laz-Theophile"
},
{
"family_name": "Liu",
"given_name": "Chang",
"orcid": "0000-0002-7866-4531"
},
{
"family_name": "Meynardie",
"given_name": "William",
"orcid": "0009-0001-6903-0131",
"clpid": "Meynardie-William"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Nir",
"given_name": "Guy",
"orcid": "0000-0002-7501-5579"
},
{
"family_name": "Patra",
"given_name": "Kishore C.",
"orcid": "0000-0002-1092-6806"
},
{
"family_name": "Pessi",
"given_name": "Priscila J.",
"orcid": "0000-0002-8041-8559"
},
{
"family_name": "Rich",
"given_name": "R. Michael",
"orcid": "0000-0003-0427-8387"
},
{
"family_name": "Rehemtulla",
"given_name": "Nabeel",
"orcid": "0000-0002-5683-2389"
},
{
"family_name": "Rose",
"given_name": "Sam",
"orcid": "0000-0003-4725-4481",
"clpid": "Rose-Sam"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Singh",
"given_name": "Avinash",
"orcid": "0000-0003-2091-622X"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert"
},
{
"family_name": "Mandigo-Stoba",
"given_name": "Milan Sharma",
"orcid": "0000-0003-1118-3132"
},
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Qin",
"given_name": "Yu-Jing",
"orcid": "0000-0003-3658-6026",
"clpid": "Qin-Yu-Jing"
},
{
"family_name": "Wise",
"given_name": "Jacob",
"orcid": "0000-0003-0733-2916"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yang",
"given_name": "Yi"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509"
},
{
"family_name": "Zimmerman",
"given_name": "Erez",
"orcid": "0000-0001-8985-2493"
}
],
"abstract": "We present the luminosity function and volumetric rate of a sample of Type IIP supernovae (SNe) from the Zwicky Transient Facility Census of the Local Universe survey (CLU). This is the largest sample of Type IIP SNe from a systematic volume-limited survey to-date. The final sample includes 330 Type IIP SNe and 36 low-luminosity Type II (LLIIP) SNe with Mr,peak > −16 mag, which triples the literature sample of LLIIP SNe. The fraction of LLIIP SNe is 19\u207a³\u208b\u2084% of the total CLU Type IIP SNe population (8\u207a¹\u208b\u2082% of all core-collapse SNe). This implies that while LLIIP SNe likely represent the fate of core-collapse SNe of 8–12 M\u2299 progenitors, they alone cannot account for the fate of all massive stars in this mass range. To derive an absolute rate, we estimate the ZTF pipeline efficiency as a function of the apparent magnitude and the local surface brightness. We derive a volumetric rate of (3.9^(+0.4)_(−0.4)) × 10\u2074 Gpc\u207b³ yr\u207b¹ for Type IIP SNe and (7.3^(+0.6)_(-0.6) x 10³ Gpc\u207b³ yr\u207b¹ for LLIIP SNe. Now that the rate of LLIIP SNe is robustly derived, the unresolved discrepancy between core-collapse SN rates and star formation rates cannot be explained by LLIIP SNe alone.
",
"doi": "10.1088/1538-3873/adcaeb",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2025-04",
"series_number": "4",
"volume": "137",
"issue": "4",
"pages": "044203"
},
{
"id": "authors:msjpj-n0609",
"collection": "authors",
"collection_id": "msjpj-n0609",
"cite_using_url": "https://authors.library.caltech.edu/records/msjpj-n0609",
"type": "article",
"title": "Sample of hydrogen-rich superluminous supernovae from the Zwicky Transient Facility",
"author": [
{
"family_name": "Pessi",
"given_name": "P. J.",
"orcid": "0000-0002-8041-8559"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Gkini",
"given_name": "A.",
"orcid": "0009-0000-9383-2305"
},
{
"family_name": "Gangopadhyay",
"given_name": "A.",
"orcid": "0000-0002-3884-5637"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Chen",
"given_name": "T.-W.",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Hinds",
"given_name": "K. R.",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Brennan",
"given_name": "S. J.",
"orcid": "0000-0003-1325-6235"
},
{
"family_name": "Hu",
"given_name": "Y.",
"orcid": "0000-0002-9744-3910"
},
{
"family_name": "Singh",
"given_name": "A.",
"orcid": "0000-0003-2091-622X"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Ho",
"given_name": "A. Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "van Velzen",
"given_name": "S."
},
{
"family_name": "Kangas",
"given_name": "T."
},
{
"family_name": "Wold",
"given_name": "A.",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "J. S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
}
],
"abstract": "Context. Hydrogen-rich superluminous supernovae (SLSNe II) are rare. The exact mechanism producing their extreme light curve peaks is not understood. Analysis of single events and small samples suggest that circumstellar material (CSM) interaction is the main mechanism responsible for the observed features. However, other mechanisms cannot be discarded. Large sample analysis can provide clarification. Aims. We aim to characterize the light curves of a sample of 107 SLSNe II to provide valuable information that can be used to validate theoretical models. Methods. We analyzed the gri light curves of SLSNe II obtained through ZTF. We studied the peak absolute magnitudes and characteristic timescales. When possible, we computed the g\u2005−\u2005r colors and pseudo-bolometric light curves, and estimated lower limits for their total radiated energy. We also studied the luminosity distribution of our sample and estimated the fraction that would be observable by the LSST. Finally, we compared our sample to other H-rich SNe and to H-poor SLSNe I. Results. SLSNe II are heterogeneous. Their median peak absolute magnitude is ∼\u2005−\u200520.3 mag in optical bands. Their rise can take from ∼two weeks to over three months, and their decline times range from ∼twenty days to over a year. We found no significant correlations between peak magnitude and timescales. SLSNe II tend to show fainter peaks, longer declines, and redder colors than SLSNe I. Conclusions. We present the largest sample of SLSN II light curves to date, comprising 107 events. Their diversity could be explained by different CSM morphologies, although theoretical analysis is needed to explore alternative scenarios. Other luminous transients, such as active galactic nuclei, tidal disruption events or SNe Ia-CSM, can easily become contaminants. Thus, good multiwavelength light curve coverage becomes paramount. LSST could miss ∼30% of the ZTF events in its gri band footprint.
",
"doi": "10.1051/0004-6361/202452014",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-03",
"volume": "695",
"pages": "A142"
},
{
"id": "authors:s8701-8ex22",
"collection": "authors",
"collection_id": "s8701-8ex22",
"cite_using_url": "https://authors.library.caltech.edu/records/s8701-8ex22",
"type": "article",
"title": "Prospects for Systematic Planetary Nebulae Detection with the Census of the Local Universe Narrowband Survey",
"author": [
{
"family_name": "Du",
"given_name": "Rong",
"orcid": "0009-0006-6543-6333",
"clpid": "Du-Rong"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Bhattacharjee",
"given_name": "Soumyadeep",
"orcid": "0000-0003-2071-2956",
"clpid": "Bhattacharjee-Soumyadeep"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Zhang",
"given_name": "Chaoran",
"orcid": "0000-0002-0331-6727"
}
],
"abstract": "\n
We investigate the efficacy of a systematic planetary nebula (PN) search in the Census of the Local Universe (CLU) narrowband (Hα) survey that covers a considerably larger sky region of above decl. −20° than most previous surveys. Using PNe observed by the Isaac Newton Telescope Photometric Hα Survey as validation, we are able to visually recover 432 out of 441 cataloged PNe (98%) within the CLU data set, with 5 sources having unusable CLU images and 4 missed due to limitations of imaging quality. Moreover, the reference PNe are conventionally divided into three PN classes in decreasing order of identification confidence given their spectra and morphologies. We record consistently high recovery rate across all classes: 95% of True, 71% of Likely, and 81% of Possible sources are readily recovered. To further demonstrate the ability of CLU to find new PNe, we undertake a preliminary search of compact PNe within a sub-region of the validation catalog, mainly utilizing the significance of narrow-band colors (Σ) as a metric for identification. In a 200 deg2 region, we search the CLU source catalog and find 31 PN candidates after automated and visual scrutiny, of which 12 are new sources not appearing in previous studies. As a demonstration of our ongoing follow-up campaign, we present medium-resolution optical spectra of six candidates and notice that four of them show emission signatures characteristic of confirmed PNe. As we refine our selection methods, CLU promises to provide a systematic catalog of PNe spanning 2/3 of the sky.
\n
During the first half of the fourth observing run (O4a) of the International Gravitational Wave Network, the Zwicky Transient Facility (ZTF) conducted a systematic search for kilonova (KN) counterparts to binary neutron star (BNS) and neutron star\u2013black hole (NSBH) merger candidates. Here, we present a comprehensive study of the five high-significance (False Alarm Rate less than 1 yr\u22121) BNS and NSBH candidates in O4a. Our follow-up campaigns relied on both target-of-opportunity observations and re-weighting of the nominal survey schedule to maximize coverage. We describe the toolkit we have been developing, Fritz, an instance of SkyPortal, instrumental in coordinating and managing our telescope scheduling, candidate vetting, and follow-up observations through a user-friendly interface. ZTF covered a total of 2841 deg2 within the skymaps of the high-significance GW events, reaching a median depth of g \u2248 20.2 mag. We circulated 15 candidates, but found no viable KN counterpart to any of the GW events. Based on the ZTF non-detections of the high-significance events in O4a, we used a Bayesian approach, nimbus, to quantify the posterior probability of KN model parameters that are consistent with our non-detections. Our analysis favors KNe with initial absolute magnitude fainter than \u221216 mag. The joint posterior probability of a GW170817-like KN associated with all our O4a follow-ups was 64%. Additionally, we use a survey simulation software, simsurvey, to determine that our combined filtered efficiency to detect a GW170817-like KN is 36%, when considering the 5 confirmed astrophysical events in O3 (1 BNS and 4 NSBH events), along with our O4a follow-ups. Following Kasliwal et al., we derived joint constraints on the underlying KN luminosity function based on our O3 and O4a follow-ups, determining that no more than 76% of KNe fading at 1 mag day\u22121 can peak at a magnitude brighter than \u221217.5 mag.
",
"doi": "10.1088/1538-3873/ad8265",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2024-11-01",
"series_number": "11",
"volume": "136",
"issue": "11",
"pages": "114201"
},
{
"id": "authors:acy4v-k2640",
"collection": "authors",
"collection_id": "acy4v-k2640",
"cite_using_url": "https://authors.library.caltech.edu/records/acy4v-k2640",
"type": "article",
"title": "A Tale of Three Dwarfs: Cluster-based Star Formation Histories of Blue Compact Dwarf Galaxies",
"author": [
{
"family_name": "Chandar",
"given_name": "Rupali",
"orcid": "0000-0003-0085-4623",
"clpid": "Chandar-Rupali"
},
{
"family_name": "Caputo",
"given_name": "Miranda",
"orcid": "0000-0002-2957-3924",
"clpid": "Caputo-Miranda"
},
{
"family_name": "Mok",
"given_name": "Angus",
"orcid": "0000-0001-7413-7534",
"clpid": "Mok-Angus"
},
{
"family_name": "Linden",
"given_name": "Sean",
"orcid": "0000-0002-1000-6081",
"clpid": "Linden-Sean"
},
{
"family_name": "Whitmore",
"given_name": "Bradley C.",
"orcid": "0000-0002-3784-7032",
"clpid": "Whitmore-Bradley-C"
},
{
"family_name": "Goudfrooij",
"given_name": "Paul",
"orcid": "0000-0002-5728-1427",
"clpid": "Goudfrooij-Paul"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-Daniela"
},
{
"family_name": "Elmegreen",
"given_name": "Debra M.",
"orcid": "0000-0002-1392-3520",
"clpid": "Elmegreen-Debra-M"
},
{
"family_name": "Lee",
"given_name": "Janice C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "\u00dabeda",
"given_name": "Leonardo",
"orcid": "0000-0001-7130-2880",
"clpid": "\u00dabeda-Leonardo"
},
{
"family_name": "White",
"given_name": "Richard",
"orcid": "0000-0002-9194-2807",
"clpid": "White-Richard"
}
],
"abstract": "\n
We present a new study of the cluster populations in the blue compact dwarf galaxies (BCD) ESO185-IG13, ESO338-IG04, and Haro11, based on new and archival high-resolution images taken by the Hubble Space Telescope, and the first to probe the populations older than ≈100 Myr. BCDs are believed to experience intense bursts of star formation (including at the present day) after long periods of quiescence, but little is known about the timing, frequency, duration, and strength of these bursts or about their star formation histories in general. We find that the cluster population in each of the three galaxies studied here has its own unique distribution of colors and hence a unique cluster and star formation history. From an assumed correlation between the normalization of the cluster mass function and the star formation rate of the host galaxy, we construct cluster-based star formation histories over the past ≈few × Gyr and find that only Haro11 is currently experiencing a burst (≈factor of 10 increase in the rate of star formation for the last ≈20 Myr), whereas ESO185 experienced enhanced star formation (by a factor ≈4) between 10 and 40 Myr ago, and ESO338 has had a fairly constant SFH over the past few Gyr. These findings indicate that not all BCDs are experiencing a burst of star formation at the present day, and that some have been forming stars and clusters at a fairly steady rate (within a factor of ≈2–3) over the past few Gyr. This scenario is similar to the histories of dwarf irregular and dwarf starburst galaxies, which have star formation rates that are 10–1000 times lower than those in BCDs.
\n
\n
SN 1987A was an unusual hydrogen-rich core-collapse supernova originating from a blue supergiant star. Similar blue supergiant explosions remain a small family of events, and are broadly characterized by their long rises to peak. The Zwicky Transient Facility Census of the Local Universe (CLU) experiment aims to construct a spectroscopically complete sample of transients occurring in galaxies from the CLU galaxy catalog. We identify 13 long-rising (>40 days) Type II supernovae from the volume-limited CLU experiment during a 3.5 yr period from 2018 June to 2021 December, approximately doubling the previously known number of these events. We present photometric and spectroscopic data of these 13 events, finding peak r-band absolute magnitudes ranging from −15.6 to −17.5 mag and the tentative detection of Ba ii lines in nine events. Using our CLU sample of events, we derive a long-rising Type II supernova rate of 1.37_(−0.30)^(+0.26) × 10\u207b\u2076 Mpc−3 yr−1, ≈1.4% of the total core-collapse supernova rate. This is the first volumetric rate of these events estimated from a large, systematic, volume-limited experiment.
\n
The vast majority of extragalactic compact continuum radio sources are associated with star formation or jets from (super)massive black holes and, as such, are more likely to be found in association with starburst galaxies or early-type galaxies. Two new populations of radio sources were recently identified: (a) compact and persistent sources (PRSs) associated with fast radio bursts (FRBs) in dwarf galaxies and (b) compact sources in dwarf galaxies that could belong to the long-sought population of intermediate-mass black holes. Despite the interesting aspects of these newly found sources, the current sample size is small, limiting scrutiny of the underlying population. Here, we present a search for compact radio sources coincident with dwarf galaxies. We search the LOFAR Two-meter Sky Survey (LoTSS), the most sensitive low-frequency (144 MHz central frequency) large-area survey for optically thin synchrotron emission to date. Exploiting the high spatial resolution (6″) and low astrometric uncertainty (∼0.″2) of the LoTSS, we match its compact sources to the compiled sample of dwarf galaxies in the Census of the Local Universe, an Hα survey with the Palomar Observatory 48 inch Samuel Oschin Telescope. We identify 29 over-luminous compact radio sources, evaluate the probability of chance alignment within the sample, investigate the potential nature of these sources, and evaluate their volumetric density and volumetric rate. While optical line-ratio diagnostics on the nebular lines from the host galaxies support a star-formation origin rather than an AGN origin, future high-angular-resolution radio data are necessary to ascertain the origin of the radio sources. We discuss planned strategies to differentiate between candidate FRB hosts and intermediate-mass black holes.
",
"doi": "10.1051/0004-6361/202346471",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2023-12",
"volume": "680",
"pages": "A98"
},
{
"id": "authors:ex29t-xd563",
"collection": "authors",
"collection_id": "ex29t-xd563",
"cite_using_url": "https://authors.library.caltech.edu/records/ex29t-xd563",
"type": "article",
"title": "Completeness of the NASA/IPAC Extragalactic Database (NED) Local Volume Sample",
"author": [
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Mazzarella",
"given_name": "J. M.",
"orcid": "0000-0002-8204-8619",
"clpid": "Mazzarella-Joseph-M"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Alcala",
"given_name": "A.",
"clpid": "Alcala-A"
},
{
"family_name": "Chen",
"given_name": "T. X.",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-X"
},
{
"family_name": "Ebert",
"given_name": "R.",
"orcid": "0000-0002-9500-8587",
"clpid": "Ebert-Rick"
},
{
"family_name": "Frayer",
"given_name": "C.",
"clpid": "Frayer-C"
},
{
"family_name": "Kim",
"given_name": "J.",
"clpid": "Kim-J"
},
{
"family_name": "Lo",
"given_name": "T.",
"clpid": "Lo-T"
},
{
"family_name": "Madore",
"given_name": "B. F.",
"orcid": "0000-0002-1576-1676"
},
{
"family_name": "Ogle",
"given_name": "P. M.",
"orcid": "0000-0002-3471-981X"
},
{
"family_name": "Schmitz",
"given_name": "M.",
"orcid": "0000-0002-2055-7549",
"clpid": "Schmitz-Marion"
},
{
"family_name": "Singer",
"given_name": "L. P.",
"orcid": "0000-0001-9898-5597"
},
{
"family_name": "Terek",
"given_name": "S.",
"clpid": "Terek-S"
},
{
"family_name": "Valladon",
"given_name": "J.",
"orcid": "0000-0001-7237-3787"
},
{
"family_name": "Wu",
"given_name": "X.",
"orcid": "0000-0002-4788-9236",
"clpid": "Wu-Xiuqin"
}
],
"abstract": "We introduce the NASA/IPAC Extragalactic Database (NED) Local Volume Sample (NED-LVS), a subset of ∼1.9 million objects with distances out to 1000 Mpc. We use UV and IR fluxes available in NED from all-sky surveys to derive physical properties, and estimate the completeness relative to the expected local luminosity density. The completeness relative to near-IR luminosities (which traces a galaxy's stellar mass) is roughly 100% at D < 30 Mpc and remains moderate (70%) out to 300 Mpc. For brighter galaxies (\u2273L *), NED-LVS is ∼100% complete out to ∼400 Mpc. When compared to other local Universe samples (GLADE and HECATE), all three are ∼100% complete below 30 Mpc. At distances beyond ∼80 Mpc, NED-LVS is more complete than both GLADE and HECATE by ∼10%–20%. NED-LVS is the underlying sample for the NED gravitational-wave follow-up service (NED-GWF), which provides prioritized lists of host candidates for GW events within minutes of alerts issued by the LIGO–Virgo–KAGRA collaboration. We test the prioritization of galaxies in the volume of GW170817 by three physical properties, where we find that both stellar mass and inverse specific star formation rate place the correct host galaxy in the top 10. In addition, NED-LVS can be used for a wide variety of other astrophysical studies: galaxy evolution, star formation, large-scale structure, galaxy environments, and more. The data in NED are updated regularly, and NED-LVS will be updated concurrently. Consequently, NED-LVS will continue to provide an increasingly complete sample of galaxies for a multitude of astrophysical research areas for years to come.
",
"doi": "10.3847/1538-4365/acdd06",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2023-09",
"series_number": "1",
"volume": "268",
"issue": "1",
"pages": "14"
},
{
"id": "authors:gdhm8-x0y60",
"collection": "authors",
"collection_id": "gdhm8-x0y60",
"cite_using_url": "https://authors.library.caltech.edu/records/gdhm8-x0y60",
"type": "article",
"title": "Constraining the LyC escape fraction from LEGUS star clusters with SIGNALS H ii region observations: a pilot study of NGC 628",
"author": [
{
"family_name": "Teh",
"given_name": "Jia Wei",
"orcid": "0000-0001-7863-5047"
},
{
"family_name": "Grasha",
"given_name": "Kathryn",
"orcid": "0000-0002-3247-5321"
},
{
"family_name": "Krumholz",
"given_name": "Mark R",
"orcid": "0000-0003-3893-854X"
},
{
"family_name": "Battisti",
"given_name": "Andrew J",
"orcid": "0000-0003-4569-2285"
},
{
"family_name": "Calzetti",
"given_name": "Daniela"
},
{
"family_name": "Rousseau-Nepton",
"given_name": "Laurie",
"orcid": "0000-0002-5136-6673"
},
{
"family_name": "Rhea",
"given_name": "Carter",
"orcid": "0000-0003-2001-1076"
},
{
"family_name": "Adamo",
"given_name": "Angela",
"orcid": "0000-0002-8192-8091"
},
{
"family_name": "Kennicutt",
"given_name": "Robert C",
"orcid": "0000-0001-5448-1821"
},
{
"family_name": "Grebel",
"given_name": "Eva K",
"orcid": "0000-0002-1891-3794"
},
{
"family_name": "Cook",
"given_name": "David O",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Combes",
"given_name": "Francoise",
"orcid": "0000-0003-2658-7893"
},
{
"family_name": "Messa",
"given_name": "Matteo",
"orcid": "0000-0003-1427-2456"
},
{
"family_name": "Linden",
"given_name": "Sean T",
"orcid": "0000-0002-1000-6081"
},
{
"family_name": "Klessen",
"given_name": "Ralf S",
"orcid": "0000-0002-0560-3172"
},
{
"family_name": "Vilchez",
"given_name": "Jos\u00e9 M",
"orcid": "0000-0001-7299-8373"
},
{
"family_name": "Fumagalli",
"given_name": "Michele",
"orcid": "0000-0001-6676-3842"
},
{
"family_name": "McLeod",
"given_name": "Anna",
"orcid": "0000-0002-5456-523X"
},
{
"family_name": "Smith",
"given_name": "Linda J",
"orcid": "0000-0002-0806-168X"
},
{
"family_name": "Chemin",
"given_name": "Laurent",
"orcid": "0000-0002-3834-7937"
},
{
"family_name": "Wang",
"given_name": "Junfeng",
"orcid": "0000-0002-7197-7404"
},
{
"family_name": "Sabbi",
"given_name": "Elena",
"orcid": "0000-0003-2954-7643"
},
{
"family_name": "Sacchi",
"given_name": "Elena",
"orcid": "0000-0001-5618-0109"
},
{
"family_name": "Petric",
"given_name": "Andreea",
"orcid": "0000-0003-4030-3455"
},
{
"family_name": "Bruna",
"given_name": "Lorenza Della"
},
{
"family_name": "Boselli",
"given_name": "Alessandro",
"orcid": "0000-0002-9795-6433"
}
],
"abstract": "The ionizing radiation of young and massive stars is a crucial form of stellar feedback. Most ionizing (Lyman-continuum; LyC, λ < 912Å) photons are absorbed close to the stars that produce them, forming compact H ii regions, but some escape into the wider galaxy. Quantifying the fraction of LyC photons that escape is an open problem. In this work, we present a seminovel method to estimate the escape fraction by combining broadband photometry of star clusters from the Legacy ExtraGalactic UV Survey (LEGUS) with H ii regions observed by the Star formation, Ionized gas, and Nebular Abundances Legacy Survey (SIGNALS) in the nearby spiral galaxy NGC 628. We first assess the completeness of the combined catalogue, and find that 49 per cent of H ii regions lack corresponding star clusters as a result of a difference in the sensitivities of the LEGUS and SIGNALS surveys. For H ii regions that do have matching clusters, we infer the escape fraction from the difference between the ionizing power required to produce the observed H ii luminosity and the predicted ionizing photon output of their host star clusters; the latter is computed using a combination of LEGUS photometric observations and a stochastic stellar population synthesis code slug (Stochastically Lighting Up Galaxies). Overall, we find an escape fraction of ${f}_{\\textrm {esc}}= 0.09^{+0.06}_{-0.06}$ across our sample of 42 H ii regions; in particular, we find H ii regions with high fesc are predominantly regions with low $\\operatorname{H\\alpha }$-luminosity. We also report possible correlation between fesc and the emission lines $\\rm [O\\, \\rm {\\small II}]/[N\\, \\rm {\\small II}]$ and $\\rm [O\\, \\rm {\\small II}]/H\\beta$.
",
"doi": "10.1093/mnras/stad1780",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2023-09",
"series_number": "1",
"volume": "524",
"issue": "1",
"pages": "1191-1210"
},
{
"id": "authors:mz8a6-0tc05",
"collection": "authors",
"collection_id": "mz8a6-0tc05",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230612-735327000.26",
"type": "article",
"title": "Volumetric Rates of Luminous Red Novae and Intermediate-luminosity Red Transients with the Zwicky Transient Facility",
"author": [
{
"family_name": "Karambelkar",
"given_name": "Viraj R.",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Blagorodnova",
"given_name": "Nadejda",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-Nadejda"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Aloisi",
"given_name": "Robert",
"orcid": "0000-0003-2822-616X",
"clpid": "Aloisi-Robert"
},
{
"family_name": "Anand",
"given_name": "Shreya G.",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya-G"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502",
"clpid": "Brink-Thomas-G"
},
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0001-8208-2473",
"clpid": "Bruch-Rachel-J"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Das",
"given_name": "Kaustav Kashyap",
"orcid": "0000-0001-8372-997X",
"clpid": "Das-Kaustav-Kashyap"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Filippenko",
"given_name": "Alexei V.",
"orcid": "0000-0003-3460-0103",
"clpid": "Filippenko-Alexei-V"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-Jacob-E"
},
{
"family_name": "Jones",
"given_name": "David",
"orcid": "0000-0003-3947-5946",
"clpid": "Jones-David"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Patra",
"given_name": "Kishore C.",
"orcid": "0000-0002-1092-6806",
"clpid": "Patra-Kishore-C"
},
{
"family_name": "Purdum",
"given_name": "Josiah N.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Reedy",
"given_name": "Alexander",
"clpid": "Reedy-Alexander"
},
{
"family_name": "Sit",
"given_name": "Tawny",
"orcid": "0000-0001-8208-9755",
"clpid": "Sit-Tawny"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "van der Walt",
"given_name": "St\u00e9fan J.",
"orcid": "0000-0001-9276-1891",
"clpid": "van-der-Walt-St\u00e9fan-J"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Zhang",
"given_name": "Chaoran",
"orcid": "0000-0002-0331-6727",
"clpid": "Zhang-Chaoran"
}
],
"abstract": "Luminous red novae (LRNe) are transients characterized by low luminosities and expansion velocities, and they are associated with mergers or common-envelope ejections in stellar binaries. Intermediate-luminosity red transients (ILRTs) are an observationally similar class with unknown origins, but they are generally believed to be either electron-capture supernovae in super-asymptotic giant branch stars or outbursts in dusty luminous blue variables (LBVs). In this paper, we present a systematic sample of eight LRNe and eight ILRTs detected as part of the Census of the Local Universe (CLU) experiment on the Zwicky Transient Facility (ZTF). The CLU experiment spectroscopically classifies ZTF transients associated with nearby (<150 Mpc) galaxies, achieving 80% completeness for mr < 20 mag. Using the ZTF-CLU sample, we derive the first systematic LRNe volumetric rate of 7.8_(-3.7)^(+6.5) x 10\u207b\u2075 Mpc\u207b\u00b3 yr\u207b\u00b9 in the luminosity range \u221216 \u2264 M\u1d63 \u2264 \u221211 mag. We find that, in this luminosity range, the LRN rate scales as dN/dL \u221d L^(-2.5 \u00b1 0.3) \u2014 significantly steeper than the previously derived scaling of L^(\u22121.4 \u00b1 0.3) for lower-luminosity LRNe (M\u1d65 \u2265 \u221210 mag). The steeper power law for LRNe at high luminosities is consistent with the massive merger rates predicted by binary population synthesis models. We find that the rates of the brightest LRNe (M\u1d63 \u2264 \u221213 mag) are consistent with a significant fraction of them being progenitors of double compact objects that merge within a Hubble time. For ILRTs, we derive a volumetric rate of 2.6_(-1.4)^(+1.8) x 10^\u207b\u2076 Mpc\u207b\u00b3 yr\u207b\u00b9 for M\u1d63 \u2264 \u221213.5 mag, which scales as dN}/dL \u221d L^(-2.5 \u00b1 0.5). This rate is \u223c1%\u20135% of the local core-collapse supernova rate and is consistent with theoretical ECSN rate estimates.",
"doi": "10.3847/1538-4357/acc2b9",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-05-10",
"series_number": "2",
"volume": "948",
"issue": "2",
"pages": "Art. No. 137"
},
{
"id": "authors:m5ax9-gtc13",
"collection": "authors",
"collection_id": "m5ax9-gtc13",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230307-206415500.29",
"type": "article",
"title": "Fraction of stars in clusters for the LEGUS dwarf galaxies",
"author": [
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Lee",
"given_name": "J. C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-Daniela"
},
{
"family_name": "Chandar",
"given_name": "R.",
"orcid": "0000-0003-0085-4623",
"clpid": "Chandar-Rupali"
},
{
"family_name": "Whitmore",
"given_name": "B. C.",
"orcid": "0000-0002-3784-7032",
"clpid": "Whitmore-Bradley-C"
},
{
"family_name": "Aloisi",
"given_name": "A.",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-Alessandra"
},
{
"family_name": "Cignoni",
"given_name": "M.",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-Michele"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-Daniel-A"
},
{
"family_name": "Elmegreen",
"given_name": "B. G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-Bruce-G"
},
{
"family_name": "Fumagalli",
"given_name": "M.",
"orcid": "0000-0001-6676-3842",
"clpid": "Fumagalli-Michele"
},
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-Kathryn"
},
{
"family_name": "Johnson",
"given_name": "K. E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-Kelsey-E"
},
{
"family_name": "Kennicutt",
"given_name": "R. C.",
"orcid": "0000-0001-5448-1821",
"clpid": "Kennicutt-Robert-C"
},
{
"family_name": "Kim",
"given_name": "H.",
"clpid": "Kim-H"
},
{
"family_name": "Linden",
"given_name": "S. T.",
"orcid": "0000-0002-1000-6081",
"clpid": "Linden-Sean-T"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-Matteo"
},
{
"family_name": "\u00d6stlin",
"given_name": "G.",
"orcid": "0000-0002-3005-1349",
"clpid": "\u00d6stlin-G\u00f6ran"
},
{
"family_name": "Ryon",
"given_name": "J. E.",
"clpid": "Ryon-Jenna-E"
},
{
"family_name": "Sacchi",
"given_name": "E.",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-Elena"
},
{
"family_name": "Thilker",
"given_name": "D. A.",
"orcid": "0000-0002-8528-7340",
"clpid": "Thilker-David-A"
},
{
"family_name": "Tosi",
"given_name": "M.",
"orcid": "0000-0002-0986-4759",
"clpid": "Tosi-Monica"
},
{
"family_name": "Wofford",
"given_name": "A.",
"orcid": "0000-0001-8289-3428",
"clpid": "Wofford-Aida"
}
],
"abstract": "We study the young star cluster populations in 23 dwarf and irregular galaxies observed by the Hubble Space Telescope (HST) Legacy ExtraGalactic Ultraviolet Survey (LEGUS), and examine relationships between the ensemble properties of the cluster populations and those of their host galaxies: star formation rate (SFR) density (\u03a3_(SFR)). A strength of this analysis is the availability of SFRs measured from temporally resolved star formation histories that provide the means to match cluster and host galaxy properties on several time-scales (1\u201310, 1\u2013100, and 10\u2013100\u00a0Myr). Nevertheless, studies of this kind are challenging for dwarf galaxies due to the small numbers of clusters in each system. We mitigate these issues by combining the clusters across different galaxies with similar \u03a3_(SFR) properties. We find good agreement with a well-established relationship (M_V^(brightest)\u2013SFR), but find no significant correlations between \u03a3_(SFR) and the slopes of the cluster luminosity function, mass function, nor the age distribution. We also find no significant trend between the fraction of stars in bound clusters at different age ranges (\u0393\u2081\u208b\u2081\u2080, \u0393\u2081\u2080\u208b\u2081\u2080\u2080, and \u0393\u2081\u208b\u2081\u2080\u2080) and \u03a3_(SFR) of the host galaxy. Our data show a decrease in \u0393 over time (from 1\u201310 to 10\u2013100\u00a0Myr) suggesting early cluster dissolution, though the presence of unbound clusters in the youngest time bin makes it difficult to quantify the degree of dissolution. While our data do not exhibit strong correlations between \u03a3_(SFR) and ensemble cluster properties, we cannot rule out that a weak trend might exist given the relatively large uncertainties due to low number statistics and the limited \u03a3_(SFR) range probed.",
"doi": "10.1093/mnras/stac3748",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2023-03",
"series_number": "3",
"volume": "519",
"issue": "3",
"pages": "3749-3775"
},
{
"id": "authors:etk73-92h24",
"collection": "authors",
"collection_id": "etk73-92h24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230221-19411400.42",
"type": "article",
"title": "Arp 220: A Post-starburst Galaxy with Little Current Star Formation outside of Its Nuclear Disks",
"author": [
{
"family_name": "Chandar",
"given_name": "Rupali",
"orcid": "0000-0003-0085-4623",
"clpid": "Chandar-Rupali"
},
{
"family_name": "Caputo",
"given_name": "Miranda",
"orcid": "0000-0002-2957-3924",
"clpid": "Caputo-Miranda"
},
{
"family_name": "Linden",
"given_name": "Sean T.",
"orcid": "0000-0002-1000-6081",
"clpid": "Linden-Sean-T"
},
{
"family_name": "Mok",
"given_name": "Angus",
"orcid": "0000-0001-7413-7534",
"clpid": "Mok-Angus"
},
{
"family_name": "Whitmore",
"given_name": "Bradley C.",
"orcid": "0000-0002-3784-7032",
"clpid": "Whitmore-Bradley-C"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-Daniela"
},
{
"family_name": "Elmegreen",
"given_name": "Debra M.",
"orcid": "0000-0002-1392-3520",
"clpid": "Elmegreen-Debra-M"
},
{
"family_name": "Lee",
"given_name": "Janice C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Ubeda",
"given_name": "Leonardo",
"clpid": "Ubeda-Leonardo"
},
{
"family_name": "White",
"given_name": "Richard",
"orcid": "0000-0002-9194-2807",
"clpid": "White-Richard-L"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
}
],
"abstract": "The ultraluminous infrared galaxy Arp 220 is a late-stage merger with several tidal structures in the outskirts and two very compact, dusty nuclei that show evidence for extreme star formation and host at least one active galactic nucleus (AGN). New and archival high-resolution images taken by the Hubble Space Telescope provide a state-of-the-art view of the structures, dust, and stellar clusters in Arp 220. These images cover the near-ultraviolet, optical, and near-infrared in both broad- and narrowband filters. We find that \u223c90% of the H\u03b1 emission arises from a shock-ionized bubble emanating from the AGN in the western nucleus, while the nuclear disks dominate the Pa\u03b2 emission. Four very young (\u223c3\u20136 Myr) but lower-mass (\u227210\u2074 M_\u2299) clusters are detected in H\u03b1 within a few arcseconds of the nuclei, but they produce less than 1% of the line emission. We see little evidence for a population of massive clusters younger than 100 Myr anywhere in Arp 220, unlike previous reports in the literature. From the masses and ages of the detected clusters, we find that star formation took place more or less continuously starting approximately a few gigayears ago with a moderate rate between \u22483 and 12 M_\u2299 yr\u207b\u00b9. Approximately 100 Myr ago, star formation shut off suddenly everywhere (possibly due to a merging event), except in the nuclear disks. A very recent flicker of weak star formation produced the four young, low-mass clusters, while the rest of the galaxy appears to have remained in a post-starburst state. Cluster ages indicate that the tidal structures on the west side of the galaxy are older than those on the east side, but all appear to predate the shutoff of star formation. Arp 220 has many of the characteristics expected of a \"shocked post-starburst galaxy,\" since most of the system has been in a post-starburst state for the past \u223c100 Myr and the detected H\u03b1 emission arises from shocked rather than photoionized gas.",
"doi": "10.3847/1538-4357/acac96",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-02-01",
"series_number": "2",
"volume": "943",
"issue": "2",
"pages": "Art. No. 142"
},
{
"id": "authors:mwgc0-wnz48",
"collection": "authors",
"collection_id": "mwgc0-wnz48",
"cite_using_url": "https://authors.library.caltech.edu/records/mwgc0-wnz48",
"type": "article",
"title": "The Hydrogen-poor Superluminous Supernovae from the Zwicky Transient Facility Phase I Survey. I. Light Curves and Measurements",
"author": [
{
"family_name": "Chen",
"given_name": "Z. H.",
"orcid": "0000-0001-5175-4652",
"clpid": "Chen-Z-H"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Kangas",
"given_name": "T.",
"orcid": "0000-0002-5477-0217"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Chen",
"given_name": "T.-W.",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Taggart",
"given_name": "K.",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Hinds",
"given_name": "K. R."
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Wang",
"given_name": "X. F."
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bellm",
"given_name": "E.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "J. S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Burdge",
"given_name": "K.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-Kevin-B"
},
{
"family_name": "Burgos",
"given_name": "A."
},
{
"family_name": "Cook",
"given_name": "D.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dahiwale",
"given_name": "A.",
"clpid": "Dahiwale-Aishwarya-S"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "R.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Dugas",
"given_name": "A.",
"orcid": "0000-0001-7344-0208"
},
{
"family_name": "Frederik",
"given_name": "S."
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Graham",
"given_name": "M.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hankins",
"given_name": "M.",
"orcid": "0000-0001-9315-8437"
},
{
"family_name": "Ho",
"given_name": "A.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Jencson",
"given_name": "J.",
"orcid": "0000-0001-5754-4007"
},
{
"family_name": "Karambelkar",
"given_name": "V.",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Kasliwal",
"given_name": "M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "S.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Laher",
"given_name": "R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Taddia",
"given_name": "F.",
"orcid": "0000-0002-2387-6801"
},
{
"family_name": "Tartaglia",
"given_name": "L.",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "Thomas",
"given_name": "B. P.",
"orcid": "0000-0002-0977-1974"
},
{
"family_name": "Tzanidakis",
"given_name": "A.",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes-C"
},
{
"family_name": "Walters",
"given_name": "R.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Yang",
"given_name": "Y."
},
{
"family_name": "Yao",
"given_name": "Y. H.",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Yaron",
"given_name": "O.",
"orcid": "0000-0002-0301-8017"
}
],
"abstract": "During the Zwicky Transient Facility (ZTF) Phase I operations, 78 hydrogen-poor superluminous supernovae (SLSNe-I) were discovered in less than 3 yr, constituting the largest sample from a single survey. This paper (Paper I) presents the data, including the optical/UV light curves and classification spectra, while Paper II in this series will focus on the detailed analysis of the light curves and modeling. Our photometry is primarily taken by ZTF in the g, r, and i bands, and with additional data from other ground-based facilities and Swift. The events of our sample cover a redshift range of z = 0.06 − 0.67, with a median and 1σ error (16% and 84% percentiles) of z_(med) = 0.265^(+0.143)_(-0.135). The peak luminosity covers −22.8 mag ≤ Mg,peak ≤ −19.8 mag, with a median value of -21.48^(+1.13)_(-0.61) mag. The light curves evolve slowly with a mean rest-frame rise time of trise = 41.9 ± 17.8 days. The luminosity and timescale distributions suggest that low-luminosity SLSNe-I with a peak luminosity ∼−20 mag or extremely fast-rising events (<10 days) exist, but are rare. We confirm previous findings that slowly rising SLSNe-I also tend to fade slowly. The rest-frame color and temperature evolution show large scatters, suggesting that the SLSN-I population may have diverse spectral energy distributions. The peak rest-frame color shows a moderate correlation with the peak absolute magnitude, i.e., brighter SLSNe-I tend to have bluer colors. With optical and UV photometry, we construct the bolometric luminosity and derive a bolometric correction relation that is generally applicable for converting g, r-band photometry to the bolometric luminosity for SLSNe-I.
",
"doi": "10.3847/1538-4357/aca161",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-01-20",
"series_number": "1",
"volume": "943",
"issue": "1",
"pages": "41"
},
{
"id": "authors:5bf4t-md570",
"collection": "authors",
"collection_id": "5bf4t-md570",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220908-184102986",
"type": "article",
"title": "Star Cluster Formation and Evolution in M101: An Investigation with the Legacy Extragalactic UV Survey",
"author": [
{
"family_name": "Linden",
"given_name": "S. T.",
"orcid": "0000-0002-1000-6081",
"clpid": "Linden-S-T"
},
{
"family_name": "Perez",
"given_name": "G.",
"orcid": "0000-0003-3880-8075",
"clpid": "Perez-G"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Maji",
"given_name": "S.",
"clpid": "Maji-S"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Whitmore",
"given_name": "B. C.",
"clpid": "Whitmore-B-C"
},
{
"family_name": "Chandar",
"given_name": "R.",
"orcid": "0000-0003-0085-4623",
"clpid": "Chandar-R"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-Kathryn"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Elmegreen",
"given_name": "B. G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-B-G"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Sacchi",
"given_name": "E.",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-Elena"
},
{
"family_name": "Sabbi",
"given_name": "E.",
"orcid": "0000-0003-2954-7643",
"clpid": "Sabbi-E"
},
{
"family_name": "Grebel",
"given_name": "E. K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-Eva-K"
},
{
"family_name": "Smith",
"given_name": "L.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-Linda-J"
}
],
"abstract": "We present Hubble Space Telescope WFC3/UVIS (F275W, F336W) and ACS/WFC optical (F435W, F555W, and F814W) observations of the nearby grand-design spiral galaxy M101 as part of the Legacy Extragalactic UV Survey (LEGUS). Compact sources detected in at least four bands were classified by both human experts and the convolutional neural network StarcNet. Human experts classified the 2351 brightest sources, retrieving Nc = 965 star clusters. StarcNet, trained on LEGUS data not including M101, classified all 4725 sources detected in four bands, retrieving Nc = 2270 star clusters. The combined catalog represents the most complete census to date of compact star clusters in M101. We find that for the 2351 sources with both a visual- and machine-learning classification StarcNet is able to reproduce the human classifications at high levels of accuracy (\u223c80%\u201390%), which is equivalent to the level of agreement between human classifiers in LEGUS. The derived cluster age distribution implies a disruption rate of dN/d\u03c4 \u221d \u03c4^(\u22120.45\u00b10.14) over 10^7 < \u03c4 < 10^8.5 yr for cluster masses \u2265103.55 M_\u2299 for the central region of M101 and dN/d\u03c4 \u221d \u03c4^(\u22120.02\u00b10.15) for cluster masses \u2265103.38 M_\u2299 in the northwest region of the galaxy. The trends we recover are weaker than those of other nearby spirals (e.g., M51) and starbursts, consistent with the M101 environment having a lower-density interstellar medium, and providing evidence in favor of environmentally dependent cluster disruption in the central, southeast, and northwest regions of M101.",
"doi": "10.3847/1538-4357/ac7c07",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-08-01",
"series_number": "2",
"volume": "935",
"issue": "2",
"pages": "Art. No. 166"
},
{
"id": "authors:sbwhn-7d873",
"collection": "authors",
"collection_id": "sbwhn-7d873",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211217-233237912",
"type": "article",
"title": "Best Practices for Data Publication in the Astronomical Literature",
"author": [
{
"family_name": "Chen",
"given_name": "Tracy X.",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-Xi"
},
{
"family_name": "Schmitz",
"given_name": "Marion",
"orcid": "0000-0002-2055-7549",
"clpid": "Schmitz-Marion"
},
{
"family_name": "Mazzarella",
"given_name": "Joseph M.",
"orcid": "0000-0002-8204-8619",
"clpid": "Mazzarella-Joseph-M"
},
{
"family_name": "Wu",
"given_name": "Xiuqin",
"orcid": "0000-0002-4788-9236",
"clpid": "Wu-Xiuqin"
},
{
"family_name": "van Eyken",
"given_name": "Julian C.",
"orcid": "0000-0003-2192-5371",
"clpid": "van-Eyken-Julian-C"
},
{
"family_name": "Accomazzi",
"given_name": "Alberto",
"orcid": "0000-0002-4110-3511"
},
{
"family_name": "Akeson",
"given_name": "Rachel L.",
"orcid": "0000-0001-9674-1564",
"clpid": "Akeson-Rachel-L"
},
{
"family_name": "Allen",
"given_name": "Mark",
"orcid": "0000-0003-2168-0087",
"clpid": "Allen-Mark-G"
},
{
"family_name": "Beaton",
"given_name": "Rachael",
"orcid": "0000-0002-1691-8217"
},
{
"family_name": "Berriman",
"given_name": "G. Bruce",
"orcid": "0000-0001-8388-534X",
"clpid": "Berriman-G-Bruce"
},
{
"family_name": "Boyle",
"given_name": "Andrew W.",
"orcid": "0000-0001-6037-2971",
"clpid": "Boyle-Andrew-W"
},
{
"family_name": "Brouty",
"given_name": "Marianne",
"orcid": "0000-0002-0944-1211"
},
{
"family_name": "Chan",
"given_name": "Ben H. P.",
"clpid": "Chan-Ben-Hiu-Pan"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-Jessie-L"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Cook",
"given_name": "David",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "D'Abrusco",
"given_name": "Raffaele",
"orcid": "0000-0003-3073-0605"
},
{
"family_name": "Ebert",
"given_name": "Rick",
"orcid": "0000-0002-9500-8587",
"clpid": "Ebert-Rick"
},
{
"family_name": "Frayer",
"given_name": "Cren",
"clpid": "Frayer-Cren"
},
{
"family_name": "Fulton",
"given_name": "Benjamin J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-Benjamin-J"
},
{
"family_name": "Gelino",
"given_name": "Christopher",
"clpid": "Gelino-Christopher-R"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Henderson",
"given_name": "Calen B.",
"orcid": "0000-0001-8877-9060",
"clpid": "Henderson-Calen-B"
},
{
"family_name": "Howell",
"given_name": "Justin",
"orcid": "0000-0001-6028-8059",
"clpid": "Howell-Justin-H"
},
{
"family_name": "Kim",
"given_name": "Joyce",
"clpid": "Kim-Joyce"
},
{
"family_name": "Landais",
"given_name": "Gilles",
"orcid": "0000-0003-4868-5873"
},
{
"family_name": "Lo",
"given_name": "Tak",
"clpid": "Lo-Tak"
},
{
"family_name": "Loup",
"given_name": "C\u00e9cile"
},
{
"family_name": "Madore",
"given_name": "Barry",
"orcid": "0000-0002-1576-1676"
},
{
"family_name": "Monari",
"given_name": "Giacomo",
"orcid": "0000-0002-6863-0661"
},
{
"family_name": "Muench",
"given_name": "August",
"orcid": "0000-0003-0666-6367"
},
{
"family_name": "Oberto",
"given_name": "Ana\u00efs",
"orcid": "0000-0001-7141-1542"
},
{
"family_name": "Ocvirk",
"given_name": "Pierre",
"orcid": "0000-0002-8488-504X"
},
{
"family_name": "Peek",
"given_name": "Joshua E. G.",
"orcid": "0000-0003-4797-7030"
},
{
"family_name": "Perret",
"given_name": "Emmanuelle",
"orcid": "0000-0002-4068-8175"
},
{
"family_name": "Pevunova",
"given_name": "Olga",
"clpid": "Pevunova-Olga"
},
{
"family_name": "Ramirez",
"given_name": "Solange V."
},
{
"family_name": "Rebull",
"given_name": "Luisa",
"orcid": "0000-0001-6381-515X",
"clpid": "Rebull-Luisa-M"
},
{
"family_name": "Shemmer",
"given_name": "Ohad",
"orcid": "0000-0003-4327-1460"
},
{
"family_name": "Smale",
"given_name": "Alan",
"orcid": "0000-0001-9207-9796"
},
{
"family_name": "Tam",
"given_name": "Raymond",
"clpid": "Tam-Raymond"
},
{
"family_name": "Terek",
"given_name": "Scott",
"clpid": "Terek-Scott"
},
{
"family_name": "Van Orsow",
"given_name": "Doug",
"orcid": "0000-0001-8405-0264"
},
{
"family_name": "Vannier",
"given_name": "Patricia"
},
{
"family_name": "Wang",
"given_name": "Shin-Ywan",
"clpid": "Wang-Shin-Ywan"
}
],
"abstract": "We present an overview of best practices for publishing data in astronomy and astrophysics journals. These recommendations are intended as a reference for authors to help prepare and publish data in a way that will better represent and support science results, enable better data sharing, improve reproducibility, and enhance the reusability of data. Observance of these guidelines will also help to streamline the extraction, preservation, integration and cross-linking of valuable data from astrophysics literature into major astronomical databases, and consequently facilitate new modes of science discovery that will better exploit the vast quantities of panchromatic and multidimensional data associated with the literature. We encourage authors, journal editors, referees, and publishers to implement the best practices reviewed here, as well as related recommendations from international astronomical organizations such as the International Astronomical Union for publication of nomenclature, data, and metadata. A convenient Checklist of Recommendations for Publishing Data in the Literature (Appendix A) is included for authors to consult before the submission of the final version of their journal articles and associated data files. We recommend that publishers of journals in astronomy and astrophysics incorporate a link to this document in their Instructions to Authors.",
"doi": "10.3847/1538-4365/ac6268",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2022-05",
"series_number": "1",
"volume": "260",
"issue": "1",
"pages": "Art. No. 5"
},
{
"id": "authors:hnpcg-rsv72",
"collection": "authors",
"collection_id": "hnpcg-rsv72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220107-252979700",
"type": "article",
"title": "Synthetic photometry of OB star clusters with stochastically sampled IMFs: analysis of models and HST observations",
"author": [
{
"family_name": "Orozco-Duarte",
"given_name": "Rogelio",
"orcid": "0000-0003-2193-3005",
"clpid": "Orozco-Duarte-Rogelio"
},
{
"family_name": "Wofford",
"given_name": "Aida",
"orcid": "0000-0001-8289-3428",
"clpid": "Wofford-Aida"
},
{
"family_name": "Vidal-Garc\u00eda",
"given_name": "Alba",
"clpid": "Vidal-Garc\u00eda-Alba"
},
{
"family_name": "Bruzual",
"given_name": "Gustavo",
"clpid": "Bruzual-Gustavo"
},
{
"family_name": "Charlot",
"given_name": "Stephane",
"clpid": "Charlot-Stephane"
},
{
"family_name": "Krumholz",
"given_name": "Mark R.",
"orcid": "0000-0003-3893-854X",
"clpid": "Krumholz-Mark-R"
},
{
"family_name": "Hannon",
"given_name": "Stephen",
"orcid": "0000-0001-9628-8958",
"clpid": "Hannon-Stephen"
},
{
"family_name": "Lee",
"given_name": "Janice",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Wofford",
"given_name": "Timothy",
"clpid": "Wofford-Timothy"
},
{
"family_name": "Fumagalli",
"given_name": "Michele",
"orcid": "0000-0001-6676-3842",
"clpid": "Fumagalli-Michele"
},
{
"family_name": "Dale",
"given_name": "Daniel",
"clpid": "Dale-Daniel"
},
{
"family_name": "Messa",
"given_name": "Matteo",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-Matteo"
},
{
"family_name": "Grebel",
"given_name": "Eva K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-Eva-K"
},
{
"family_name": "Smith",
"given_name": "Linda",
"clpid": "Smith-Linda"
},
{
"family_name": "Grasha",
"given_name": "Kathryn",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-Kathryn"
},
{
"family_name": "Cook",
"given_name": "David",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
}
],
"abstract": "We present a pilot library of synthetic NUV, U, B, V, and I photometry of star clusters with stochastically sampled IMFs and ionized gas for initial masses, M_i = 10\u00b3, 10\u2074, and 10\u2075\u2009M\u2299; t = 1, 3, 4, and 8 Myr; Z = 0.014 and Z = 0.002; and log(U_S) = \u22122 and \u22123. We compare the library with predictions from deterministic models and observations of isolated low-mass (<10\u2074\u2009M\u2299) star clusters with co-spatial compact H\u2009II regions. The clusters are located in NGC 7793, one of the nearest galaxies observed as part of the HST LEGUS and H\u03b1-LEGUS surveys. (1) For model magnitudes that only account for the stars: (a) the residual |deterministic mag - median stochastic mag| can be \u22650.5 mag, even for M_i = 10\u2075\u2009M\u2299; and (b) the largest spread in stochastic magnitudes occurs when Wolf\u2013Rayet stars are present. (2) For M_i = 10\u2075\u2009M\u2299: (a) the median stochastic mag with gas can be >1.0 mag more luminous than the median stochastic magnitude without gas; and (b) nebular emission lines can contribute with >50 per cent and >30 per cent to the total emission in the V and I bands, respectively. (3) Age-dating OB-star clusters via deterministic tracks in the U-B versus V-I plane is highly uncertain at Z = 0.014 for M_i \u223c 10\u00b3\u2009M\u2299 and Z = 0.002 for M_i \u223c 10\u00b3\u201310\u2075\u2009M\u2299. (4) For low-mass clusters, the V-band extinction derived with stochastic models significantly depends on the value of log(US). (5) The youngest clusters tend to have higher extinction. (6) The majority of clusters have multi-peaked age PDFs. (7) Finally, we discuss the importance of characterizing the true variance in the number of stars per mass bin in nature.",
"doi": "10.1093/mnras/stab2988",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2022-01",
"series_number": "1",
"volume": "509",
"issue": "1",
"pages": "522-549"
},
{
"id": "authors:32754-at028",
"collection": "authors",
"collection_id": "32754-at028",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220119-572400000",
"type": "article",
"title": "Classification of Astrophysics Journal Articles with Machine Learning to Identify Data for NED",
"author": [
{
"family_name": "Chen",
"given_name": "Tracy X.",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-Xi"
},
{
"family_name": "Ebert",
"given_name": "Rick",
"orcid": "0000-0002-9500-8587",
"clpid": "Ebert-Rick-J"
},
{
"family_name": "Mazzarella",
"given_name": "Joseph M.",
"orcid": "0000-0002-8204-8619",
"clpid": "Mazzarella-Joseph-M"
},
{
"family_name": "Frayer",
"given_name": "Cren",
"clpid": "Frayer-Cren"
},
{
"family_name": "Terek",
"given_name": "Scott",
"clpid": "Terek-Scott"
},
{
"family_name": "Chan",
"given_name": "Ben H. P.",
"clpid": "Chan-Ben-Hiu-Pan"
},
{
"family_name": "Cook",
"given_name": "David",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Lo",
"given_name": "Tak",
"clpid": "Lo-Tak"
},
{
"family_name": "Schmitz",
"given_name": "Marion",
"orcid": "0000-0002-2055-7549",
"clpid": "Schmitz-Marion"
},
{
"family_name": "Wu",
"given_name": "Xiuqin",
"orcid": "0000-0002-4788-9236",
"clpid": "Wu-Xiuqin"
}
],
"abstract": "The NASA/IPAC Extragalactic Database (NED) is a comprehensive online service that combines fundamental multi-wavelength information for known objects beyond the Milky Way and provides value-added, derived quantities and tools to search and access the data. The contents and relationships between measurements in the database are continuously augmented and revised to stay current with astrophysics literature and new sky surveys. The conventional process of distilling and extracting data from the literature involves human experts to review the journal articles and determine if an article is of extragalactic nature, and if so, what types of data it contains. This is both labor intensive and unsustainable, especially given the ever-increasing number of publications each year. We present here a machine learning (ML) approach developed and integrated into the NED production pipeline to help automate the classification of journal article topics and their data content for inclusion into NED. We show that this ML application can successfully reproduce the classifications of a human expert to an accuracy of over 90% in a fraction of the time it takes a human, allowing us to focus human expertise on tasks that are more difficult to automate.",
"doi": "10.1088/1538-3873/ac3c36",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2022-01",
"series_number": "1031",
"volume": "134",
"issue": "1031",
"pages": "Art. No. 014501"
},
{
"id": "authors:r0zrd-bsk17",
"collection": "authors",
"collection_id": "r0zrd-bsk17",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211221-866893000",
"type": "article",
"title": "Testing the Relationship between Bursty Star Formation and Size Fluctuations of Local Dwarf Galaxies",
"author": [
{
"family_name": "Emami",
"given_name": "Najmeh",
"orcid": "0000-0003-2047-1689",
"clpid": "Emami-Najmeh"
},
{
"family_name": "Siana",
"given_name": "Brian",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "El-Badry",
"given_name": "Kareem",
"orcid": "0000-0002-6871-1752",
"clpid": "El-Badry-Kareem"
},
{
"family_name": "Cook",
"given_name": "David",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Ma",
"given_name": "Xiangcheng",
"orcid": "0000-0001-8091-2349",
"clpid": "Ma-Xiangcheng"
},
{
"family_name": "Weisz",
"given_name": "Daniel",
"orcid": "0000-0002-6442-6030",
"clpid": "Weisz-Daniel-R"
},
{
"family_name": "Gharibshah",
"given_name": "Joobin",
"clpid": "Gharibshah-Joobin"
},
{
"family_name": "Alaee",
"given_name": "Sara",
"orcid": "0000-0001-5870-4025",
"clpid": "Alaee-Sara"
},
{
"family_name": "Scarlata",
"given_name": "Claudia",
"orcid": "0000-0002-9136-8876",
"clpid": "Scarlata-Claudia-M"
},
{
"family_name": "Skillman",
"given_name": "Evan",
"orcid": "0000-0003-0605-8732",
"clpid": "Skillman-Evan"
}
],
"abstract": "Stellar feedback in dwarf galaxies plays a critical role in regulating star formation via galaxy-scale winds. Recent hydrodynamical zoom-in simulations of dwarf galaxies predict that the periodic outward flow of gas can change the gravitational potential sufficiently to cause radial migration of stars. To test the effect of bursty star formation on stellar migration, we examine star formation observables and sizes of 86 local dwarf galaxies. We find a correlation between the R-band half-light radius (R_e) and far-UV luminosity (L_(FUV)) for stellar masses below 10\u2078 M\u2299 and a weak correlation between the R_e and H\u03b1 luminosity (L_(H\u03b1)). We produce mock observations of eight low-mass galaxies from the FIRE-2 cosmological simulations and measure the similarity of the time sequences of R_e and a number of star formation indicators with different timescales. Major episodes of R_e time sequence align very well with the major episodes of star formation, with a delay of \u223c50 Myr. This correlation decreases toward star formation rate indicators of shorter timescales such that R_e is weakly correlated with L_(FUV) (10\u2013100 Myr timescale) and is completely uncorrelated with L_(H\u03b1) (a few Myr timescale), in agreement with the observations. Our findings based on FIRE-2 suggest that the R-band size of a galaxy reacts to star formation variations on a \u223c50 Myr timescale. With the advent of a new generation of large space telescopes (e.g., JWST), this effect can be examined explicitly in galaxies at higher redshifts, where bursty star formation is more prominent.",
"doi": "10.3847/1538-4357/ac1f8d",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-12-01",
"series_number": "2",
"volume": "922",
"issue": "2",
"pages": "Art. No. 217"
},
{
"id": "authors:frker-e8898",
"collection": "authors",
"collection_id": "frker-e8898",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211104-154229618",
"type": "article",
"title": "The dependence of the hierarchical distribution of star clusters on galactic environment",
"author": [
{
"family_name": "Menon",
"given_name": "Shyam H.",
"orcid": "0000-0001-5944-291X",
"clpid": "Menon-Shyam-H"
},
{
"family_name": "Grasha",
"given_name": "Kathryn",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-Kathryn"
},
{
"family_name": "Elmegreen",
"given_name": "Bruce G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-Bruce-G"
},
{
"family_name": "Federrath",
"given_name": "Christoph",
"orcid": "0000-0002-0706-2306",
"clpid": "Federrath-Christoph"
},
{
"family_name": "Krumholz",
"given_name": "Mark R.",
"orcid": "0000-0003-3893-854X",
"clpid": "Krumholz-Mark-R"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-Daniela"
},
{
"family_name": "S\u00e1nchez",
"given_name": "N\u00e9stor",
"orcid": "0000-0002-0042-3180",
"clpid": "S\u00e1nchez-N\u00e9stor"
},
{
"family_name": "Linden",
"given_name": "Sean T.",
"orcid": "0000-0002-1000-6081",
"clpid": "Linden-Sean-T"
},
{
"family_name": "Adamo",
"given_name": "Angela",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Messa",
"given_name": "Matteo",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-Matteo"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "Daniel A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-Daniel-A"
},
{
"family_name": "Grebel",
"given_name": "Eva K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-Eva-K"
},
{
"family_name": "Fumagalli",
"given_name": "Michele",
"orcid": "0000-0001-6676-3842",
"clpid": "Fumagalli-Michele"
},
{
"family_name": "Sabbi",
"given_name": "Elena",
"orcid": "0000-0003-2954-7643",
"clpid": "Sabbi-Elena"
},
{
"family_name": "Johnson",
"given_name": "Kelsey E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-Kelsey-E"
},
{
"family_name": "Smith",
"given_name": "Linda J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-Linda-J"
},
{
"family_name": "Kennicutt",
"given_name": "Robert C.",
"orcid": "0000-0001-5448-1821",
"clpid": "Kennicutt-Robert-C-Jr"
}
],
"abstract": "We use the angular two-point correlation function (TPCF) to investigate the hierarchical distribution of young star clusters in 12 local (3\u201318 Mpc) star-forming galaxies using star cluster catalogs obtained with the Hubble Space Telescope (HST) as part of the Treasury Program Legacy ExtraGalactic UV Survey. The sample spans a range of different morphological types, allowing us to infer how the physical properties of the galaxy affect the spatial distribution of the clusters. We also prepare a range of physically motivated toy models to compare with and interpret the observed features in the TPCFs. We find that, conforming to earlier studies, young clusters (\u2060T \u2272 10 Myr\u2060) have power-law TPCFs that are characteristic of fractal distributions with a fractal dimension D\u2082, and this scale-free nature extends out to a maximum scale l_(corr) beyond which the distribution becomes Poissonian. However, l_(corr), and D\u2082 vary significantly across the sample, and are correlated with a number of host galaxy physical properties, suggesting that there are physical differences in the underlying star cluster distributions. We also find that hierarchical structuring weakens with age, evidenced by flatter TPCFs for older clusters (\u2060T \u2273 10 Myr\u2060), that eventually converges to the residual correlation expected from a completely random large-scale radial distribution of clusters in the galaxy in \u223c100 Myr\u2060. Our study demonstrates that the hierarchical distribution of star clusters evolves with age, and is strongly dependent on the properties of the host galaxy environment.",
"doi": "10.1093/mnras/stab2413",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2021-11",
"series_number": "4",
"volume": "507",
"issue": "4",
"pages": "5542-5566"
},
{
"id": "authors:4pkqa-fgh95",
"collection": "authors",
"collection_id": "4pkqa-fgh95",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210222-100903009",
"type": "article",
"title": "A Comparison of Star-forming Clumps and Tidal Tails in Local Mergers and High-redshift Galaxies",
"author": [
{
"family_name": "Elmegreen",
"given_name": "Debra Meloy",
"orcid": "0000-0002-1392-3520",
"clpid": "Elmegreen-Debra-M"
},
{
"family_name": "Elmegreen",
"given_name": "Bruce G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-Bruce-G"
},
{
"family_name": "Whitmore",
"given_name": "Bradley C.",
"orcid": "0000-0002-3784-7032",
"clpid": "Whitmore-Bradley-C"
},
{
"family_name": "Chandar",
"given_name": "Rupali",
"orcid": "0000-0003-0085-4623",
"clpid": "Chandar-Rupali"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-Daniela"
},
{
"family_name": "Lee",
"given_name": "Janice C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "White",
"given_name": "Richard",
"orcid": "0000-0002-9194-2807",
"clpid": "White-Richard-L"
},
{
"family_name": "Cook",
"given_name": "David",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Ubeda",
"given_name": "Leonardo",
"clpid": "Ubeda-Leonardo"
},
{
"family_name": "Mok",
"given_name": "Angus",
"orcid": "0000-0001-7413-7534",
"clpid": "Mok-Angus"
},
{
"family_name": "Linden",
"given_name": "Sean T.",
"orcid": "0000-0002-1000-6081",
"clpid": "Linden-Sean-T"
}
],
"abstract": "The Clusters, Clumps, Dust, and Gas in Extreme Star-forming Galaxies (CCDG) survey with the Hubble Space Telescope includes multiwavelength imaging of 13 galaxies less than 100 Mpc away, spanning a range of morphologies and sizes, from blue compact dwarfs to luminous infrared galaxies, all with star formation rates in excess of hundreds of solar masses per year. Images of seven merging galaxies in the CCDG survey were artificially redshifted to compare with galaxies at z = 0.5, 1, and 2. Most redshifted tails have surface brightnesses that would be visible at z = 0.5 or 1 but not at z = 2 due to cosmological dimming. Giant star clumps are apparent in these galaxies; the 51 measured have similar sizes, masses, and colors to clumps in observed high-z systems in the UDF, GEMS, GOODS, and CANDELS surveys. These results suggest that some clumpy high-z galaxies without observable tidal features could be the result of mergers. The local clumps also have the same star formation rate per unit area and stellar surface density as clumps observed at intermediate and high redshift, so they provide insight into the substructure of distant clumps. A total of 1596 star clusters brighter than M V = \u22129 were identified within the boundaries of the local clumps. The cluster magnitude distribution function is a power law with approximately the same slope (~\u22121 for a plot of number versus log luminosity) for all the galaxies both inside and outside the clumps and independently of clump surface brightness.",
"doi": "10.3847/1538-4357/abd541",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-02-20",
"series_number": "2",
"volume": "908",
"issue": "2",
"pages": "Art. No. 121"
},
{
"id": "authors:8qy1p-5vg59",
"collection": "authors",
"collection_id": "8qy1p-5vg59",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210128-145053093",
"type": "article",
"title": "Identification of a Local Sample of Gamma-Ray Bursts Consistent with a Magnetar Giant Flare Origin",
"author": [
{
"family_name": "Burns",
"given_name": "E.",
"orcid": "0000-0002-2942-3379",
"clpid": "Burns-Eric"
},
{
"family_name": "Svinkin",
"given_name": "D.",
"orcid": "0000-0002-2208-2196"
},
{
"family_name": "Hurley",
"given_name": "K."
},
{
"family_name": "Wadiasingh",
"given_name": "Z.",
"orcid": "0000-0002-9249-0515"
},
{
"family_name": "Negro",
"given_name": "M."
},
{
"family_name": "Younes",
"given_name": "G.",
"orcid": "0000-0002-7991-028X"
},
{
"family_name": "Hamburg",
"given_name": "R.",
"clpid": "Hamburg-R"
},
{
"family_name": "Ridnaia",
"given_name": "A.",
"orcid": "0000-0001-9477-5437"
},
{
"family_name": "Cook",
"given_name": "D.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Cenko",
"given_name": "S. B.",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Aloisi",
"given_name": "R.",
"orcid": "0000-0003-2822-616X"
},
{
"family_name": "Ashton",
"given_name": "G.",
"orcid": "0000-0001-7288-2231"
},
{
"family_name": "Baring",
"given_name": "M.",
"orcid": "0000-0003-4433-1365"
},
{
"family_name": "Briggs",
"given_name": "M. S."
},
{
"family_name": "Christensen",
"given_name": "N.",
"orcid": "0000-0002-6870-4202"
},
{
"family_name": "Frederiks",
"given_name": "D.",
"orcid": "0000-0002-1153-6340"
},
{
"family_name": "Goldstein",
"given_name": "A.",
"orcid": "0000-0002-0587-7042"
},
{
"family_name": "Hui",
"given_name": "C. M.",
"orcid": "0000-0002-0468-6025"
},
{
"family_name": "Kaplan",
"given_name": "D. L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kocevski",
"given_name": "D.",
"orcid": "0000-0001-9201-4706"
},
{
"family_name": "Roberts",
"given_name": "O. J.",
"orcid": "0000-0002-7150-9061"
},
{
"family_name": "Savchenko",
"given_name": "V.",
"orcid": "0000-0001-6353-0808"
},
{
"family_name": "Tohuvavohu",
"given_name": "A.",
"orcid": "0000-0002-2810-8764"
},
{
"family_name": "Veres",
"given_name": "P.",
"orcid": "0000-0002-2149-9846"
},
{
"family_name": "Wilson-Hodge",
"given_name": "C. A.",
"orcid": "0000-0002-8585-0084"
}
],
"abstract": "Cosmological gamma-ray bursts (GRBs) are known to arise from distinct progenitor channels: short GRBs mostly from neutron star mergers and long GRBs from a rare type of core-collapse supernova (CCSN) called collapsars. Highly magnetized neutron stars called magnetars also generate energetic, short-duration gamma-ray transients called magnetar giant flares (MGFs). Three have been observed from the Milky Way and its satellite galaxies, and they have long been suspected to constitute a third class of extragalactic GRBs. We report the unambiguous identification of a distinct population of four local (<5 Mpc) short GRBs, adding GRB 070222 to previously discussed events. While identified solely based on alignment with nearby star-forming galaxies, their rise time and isotropic energy release are independently inconsistent with the larger short GRB population at >99.9% confidence. These properties, the host galaxies, and nondetection in gravitational waves all point to an extragalactic MGF origin. Despite the small sample, the inferred volumetric rates for events above 4 \u00d7 10\u2074\u2074 erg of R_(MGF) = 3.8^(+4.0)_(\u22123.1) \u00d7 10\u2075 Gpc\u207b\u00b3 yr\u207b\u00b9 make MGFs the dominant gamma-ray transient detected from extragalactic sources. As previously suggested, these rates imply that some magnetars produce multiple MGFs, providing a source of repeating GRBs. The rates and host galaxies favor common CCSN as key progenitors of magnetars.",
"doi": "10.3847/2041-8213/abd8c8",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2021-02-01",
"series_number": "2",
"volume": "907",
"issue": "2",
"pages": "Art. No. L28"
},
{
"id": "authors:6d951-rq497",
"collection": "authors",
"collection_id": "6d951-rq497",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210204-105727688",
"type": "article",
"title": "Bright, Months-long Stellar Outbursts Announce the Explosion of Interaction-powered Supernovae",
"author": [
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730",
"clpid": "Strotjohann-Nora-L"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Shaviv",
"given_name": "Nir",
"orcid": "0000-0003-3894-8422"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Filippenko",
"given_name": "Alexei V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Yaron",
"given_name": "Ofer",
"orcid": "0000-0002-0301-8017"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Perley",
"given_name": "Dan A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Yang",
"given_name": "Yi"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Barbarino",
"given_name": "Cristina",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Tartaglia",
"given_name": "Leonardo",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-Daniel-A"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Lunnan",
"given_name": "Ragnhild",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "Shri R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Nugent",
"given_name": "Peter E.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Rosnet",
"given_name": "Philippe",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Adams",
"given_name": "Scott M.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-Ashot"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-Kevin-B"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"orcid": "0000-0001-7344-0208",
"clpid": "Dugas-Alison-M"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Goldwasser",
"given_name": "Samantha"
},
{
"family_name": "Hankins",
"given_name": "Matthew",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-Matthew-J"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Liang",
"given_name": "Jingyi"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Porter",
"given_name": "Michael",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-Michael-D"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Short",
"given_name": "Phil",
"orcid": "0000-0002-5096-9464"
},
{
"family_name": "Taddia",
"given_name": "Francesco",
"orcid": "0000-0002-2387-6801"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Jan"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Zhuang",
"given_name": "Zhuyun",
"orcid": "0000-0002-1945-2299",
"clpid": "Zhuang-Zhuyun"
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],
"abstract": "Interaction-powered supernovae (SNe) explode within an optically thick circumstellar medium (CSM) that could be ejected during eruptive events. To identify and characterize such pre-explosion outbursts, we produce forced-photometry light curves for 196 interacting SNe, mostly of Type IIn, detected by the Zwicky Transient Facility between early 2018 and 2020 June. Extensive tests demonstrate that we only expect a few false detections among the 70,000 analyzed pre-explosion images after applying quality cuts and bias corrections. We detect precursor eruptions prior to 18 Type IIn SNe and prior to the Type Ibn SN 2019uo. Precursors become brighter and more frequent in the last months before the SN and month-long outbursts brighter than magnitude \u221213 occur prior to 25% (5\u201369%, 95% confidence range) of all Type IIn SNe within the final three months before the explosion. With radiative energies of up to 10\u2074\u2079 erg, precursors could eject ~1 M\u2299 of material. Nevertheless, SNe with detected precursors are not significantly more luminous than other SNe IIn, and the characteristic narrow hydrogen lines in their spectra typically originate from earlier, undetected mass-loss events. The long precursor durations require ongoing energy injection, and they could, for example, be powered by interaction or by a continuum-driven wind. Instabilities during the neon- and oxygen-burning phases are predicted to launch precursors in the final years to months before the explosion; however, the brightest precursor is 100 times more energetic than anticipated.",
"doi": "10.3847/1538-4357/abd032",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-02-01",
"series_number": "2",
"volume": "907",
"issue": "2",
"pages": "Art. No. 99"
},
{
"id": "authors:5h3j9-apc36",
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"collection_id": "5h3j9-apc36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200824-085517593",
"type": "article",
"title": "Kilonova Luminosity Function Constraints Based on Zwicky Transient Facility Searches for 13 Neutron Star Merger Triggers during O3",
"author": [
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
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{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387"
},
{
"family_name": "Sagu\u00e9s Carracedo",
"given_name": "Ana"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-Michael-W"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Kumar",
"given_name": "Harsh"
},
{
"family_name": "Almualla",
"given_name": "Mouza",
"orcid": "0000-0002-4694-7123"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
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{
"family_name": "Bulla",
"given_name": "Mattia",
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{
"family_name": "Dobie",
"given_name": "Dougal",
"orcid": "0000-0003-0699-7019"
},
{
"family_name": "Reusch",
"given_name": "Simeon"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
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{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996"
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{
"family_name": "Copperwheat",
"given_name": "Christopher M.",
"orcid": "0000-0001-7983-8698"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Anupama",
"given_name": "G. C.",
"orcid": "0000-0003-3533-7183"
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{
"family_name": "Corsi",
"given_name": "Alessandra",
"orcid": "0000-0001-8104-3536"
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{
"family_name": "Nissanke",
"given_name": "Samaya",
"orcid": "0000-0001-6573-7773"
},
{
"family_name": "Agudo",
"given_name": "Iv\u00e1n"
},
{
"family_name": "Bagdasaryan",
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{
"family_name": "Barway",
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{
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{
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"given_name": "Joshua S.",
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{
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{
"family_name": "Buckley",
"given_name": "David A. H.",
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{
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"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
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{
"family_name": "Burruss",
"given_name": "Rick",
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{
"family_name": "Caballero-Garc\u0131a",
"given_name": "Maria D.",
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{
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"given_name": "Chris",
"orcid": "0000-0003-2667-7290",
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{
"family_name": "Castro-Tirado",
"given_name": "Alberto J."
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{
"family_name": "Cook",
"given_name": "David O.",
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},
{
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{
"family_name": "Cunningham",
"given_name": "Virginia",
"orcid": "0000-0003-2292-0441"
},
{
"family_name": "Dahiwale",
"given_name": "Aishwarya",
"clpid": "Dahiwale-Aishwarya-S"
},
{
"family_name": "Deshmukh",
"given_name": "Kunal P.",
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},
{
"family_name": "Dichiara",
"given_name": "Simone",
"orcid": "0000-0001-6849-1270"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Dutta",
"given_name": "Anirban"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-Michael-E"
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{
"family_name": "Franckowiak",
"given_name": "Anna",
"orcid": "0000-0002-5605-2219"
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{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
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{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230"
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{
"family_name": "Ghosh",
"given_name": "Shaon",
"orcid": "0000-0001-9901-6253"
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{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
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{
"family_name": "Golkhou",
"given_name": "V. Zach",
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{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
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{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136",
"clpid": "Graham-Melissa-Lynn"
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{
"family_name": "Hankins",
"given_name": "Matthew J.",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-Matthew-J"
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{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
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{
"family_name": "Hu",
"given_name": "Youdong",
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{
"family_name": "Ip",
"given_name": "Wing-Huen",
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{
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},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Kong",
"given_name": "Albert K. H.",
"orcid": "0000-0002-5105-344X"
},
{
"family_name": "Kowalski",
"given_name": "Marek"
},
{
"family_name": "Khandagale",
"given_name": "Maitreya"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kumar",
"given_name": "Brajesh"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Li",
"given_name": "K. L.",
"orcid": "0000-0001-8229-2024"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Mogotsi",
"given_name": "Moses"
},
{
"family_name": "Mohite",
"given_name": "Siddharth"
},
{
"family_name": "Mooley",
"given_name": "Kunal",
"orcid": "0000-0002-2557-5180",
"clpid": "Mooley-Kunal-Prakash"
},
{
"family_name": "Mr\u00f3z",
"given_name": "Przemek",
"orcid": "0000-0001-7016-1692",
"clpid": "Mr\u00f3z-Przemek"
},
{
"family_name": "Newman",
"given_name": "Jeffrey A.",
"orcid": "0000-0001-8684-2222"
},
{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554"
},
{
"family_name": "Oates",
"given_name": "Samantha R.",
"orcid": "0000-0001-9309-7873"
},
{
"family_name": "Patil",
"given_name": "Atharva Sunil"
},
{
"family_name": "Pandey",
"given_name": "Shashi B."
},
{
"family_name": "Pavana",
"given_name": "M."
},
{
"family_name": "Pian",
"given_name": "Elena",
"orcid": "0000-0001-8646-4858"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Sanchez-Ram\u0131rez",
"given_name": "Ruben",
"orcid": "0000-0002-7158-5099"
},
{
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"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Singh",
"given_name": "Avinash"
},
{
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"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
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{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Tan",
"given_name": "Hanjie"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
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{
"family_name": "Troja",
"given_name": "Eleonora",
"orcid": "0000-0002-1869-7817"
},
{
"family_name": "Valeev",
"given_name": "Azamat F.",
"orcid": "0000-0003-3513-3527"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard"
},
{
"family_name": "Waratkar",
"given_name": "Gaurav",
"orcid": "0000-0003-3630-9440"
},
{
"family_name": "Webb",
"given_name": "Sara",
"orcid": "0000-0003-2601-1472"
},
{
"family_name": "Yu",
"given_name": "Po-Chieh",
"orcid": "0000-0001-8894-0854"
},
{
"family_name": "Zhang",
"given_name": "Bin-Bin"
},
{
"family_name": "Zhou",
"given_name": "Rongpu",
"orcid": "0000-0001-5381-4372"
},
{
"family_name": "Zolkower",
"given_name": "Jeffry",
"clpid": "Zolkower-Jeffry"
}
],
"abstract": "We present a systematic search for optical counterparts to 13 gravitational wave (GW) triggers involving at least one neutron star during LIGO/Virgo's third observing run (O3). We searched binary neutron star (BNS) and neutron star black hole (NSBH) merger localizations with the Zwicky Transient Facility (ZTF) and undertook follow-up with the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration. The GW triggers had a median localization area of 4480 deg\u00b2, a median distance of 267 Mpc, and false-alarm rates ranging from 1.5 to 10\u207b\u00b2\u2075 yr\u207b\u00b9. The ZTF coverage in the g and r bands had a median enclosed probability of 39%, median depth of 20.8 mag, and median time lag between merger and the start of observations of 1.5 hr. The O3 follow-up by the GROWTH team comprised 340 UltraViolet/Optical/InfraRed (UVOIR) photometric points, 64 OIR spectra, and three radio images using 17 different telescopes. We find no promising kilonovae (radioactivity-powered counterparts), and we show how to convert the upper limits to constrain the underlying kilonova luminosity function. Initially, we assume that all GW triggers are bona fide astrophysical events regardless of false-alarm rate and that kilonovae accompanying BNS and NSBH mergers are drawn from a common population; later, we relax these assumptions. Assuming that all kilonovae are at least as luminous as the discovery magnitude of GW170817 (\u221216.1 mag), we calculate that our joint probability of detecting zero kilonovae is only 4.2%. If we assume that all kilonovae are brighter than \u221216.6 mag (the extrapolated peak magnitude of GW170817) and fade at a rate of 1 mag day\u207b\u00b9 (similar to GW170817), the joint probability of zero detections is 7%. If we separate the NSBH and BNS populations based on the online classifications, the joint probability of zero detections, assuming all kilonovae are brighter than \u221216.6 mag, is 9.7% for NSBH and 7.9% for BNS mergers. Moreover, no more than <57% (<89%) of putative kilonovae could be brighter than \u221216.6 mag assuming flat evolution (fading by 1 mag day\u207b\u00b9) at the 90% confidence level. If we further take into account the online terrestrial probability for each GW trigger, we find that no more than <68% of putative kilonovae could be brighter than \u221216.6 mag. Comparing to model grids, we find that some kilonovae must have M_(ej) < 0.03 M_\u2299, X_(lan) > 10\u207b\u2074, or \u03c6 > 30\u00b0 to be consistent with our limits. We look forward to searches in the fourth GW observing run; even 17 neutron star mergers with only 50% coverage to a depth of \u221216 mag would constrain the maximum fraction of bright kilonovae to <25%.",
"doi": "10.3847/1538-4357/abc335",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-12-20",
"series_number": "2",
"volume": "905",
"issue": "2",
"pages": "Art. No. 145"
},
{
"id": "authors:0z0sc-hap43",
"collection": "authors",
"collection_id": "0z0sc-hap43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151423784",
"type": "article",
"title": "The Zwicky Transient Facility Census of the Local Universe. I. Systematic Search for Calcium-rich Gap Transients Reveals Three Related Spectroscopic Subclasses",
"author": [
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "Fremling",
"given_name": "U. Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Adams",
"given_name": "Scott",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Aloisi",
"given_name": "Robert",
"orcid": "0000-0003-2822-616X"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-Ashot"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bildsten",
"given_name": "Lars"
},
{
"family_name": "Cannella",
"given_name": "Christopher",
"orcid": "0000-0003-2667-7290",
"clpid": "Cannella-Christopher-B"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Delacroix",
"given_name": "Alexandre",
"clpid": "Delacroix-Alexandre"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"clpid": "Dugas-Alison-M"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Goldstein",
"given_name": "Daniel",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-Daniel-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-David-D-S"
},
{
"family_name": "Hankins",
"given_name": "Matthew",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-Matthew-J"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Kaye",
"given_name": "Stephen",
"clpid": "Kaye-Stephen"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Leadbeater",
"given_name": "Robin"
},
{
"family_name": "Lunnan",
"given_name": "Ragnhild",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-Ragnhild"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Polin",
"given_name": "Abigail",
"orcid": "0000-0002-1633-6495"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Quataert",
"given_name": "Eliot",
"orcid": "0000-0001-9185-5044"
},
{
"family_name": "Reiley",
"given_name": "Dan",
"clpid": "Reiley-Daniel-J"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Tartaglia",
"given_name": "Leonardo",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
}
],
"abstract": "Using the Zwicky Transient Facility alert stream, we are conducting a large spectroscopic campaign to construct a complete, volume-limited sample of transients brighter than 20 mag, and coincident within 100\" of galaxies in the Census of the Local Universe catalog. We describe the experiment design and spectroscopic completeness from the first 16 months of operations, which have classified 754 supernovae. We present results from a systematic search for calcium-rich gap transients in the sample of 22 low-luminosity (peak absolute magnitude M > \u221217), hydrogen-poor events found in the experiment. We report the detection of eight new events, and constrain their volumetric rate to \u2273 15% \u00b1 5% of the SN Ia rate. Combining this sample with 10 previously known events, we find a likely continuum of spectroscopic properties ranging from events with SN Ia\u2013like features (Ca-Ia objects) to those with SN Ib/c\u2013like features (Ca-Ib/c objects) at peak light. Within the Ca-Ib/c events, we find two populations distinguished by their red (g \u2212 r \u2248 1.5 mag) or green (g - r \u2248 0.5 mag) colors at the r-band peak, wherein redder events show strong line blanketing features and slower light curves (similar to Ca-Ia objects), weaker He lines, and lower [Ca ii]/[O i] in the nebular phase. We find that all together the spectroscopic continuum, volumetric rates, and striking old environments are consistent with the explosive burning of He shells on low-mass white dwarfs. We suggest that Ca-Ia and red Ca-Ib/c objects arise from the double detonation of He shells, while green Ca-Ib/c objects are consistent with low-efficiency burning scenarios like detonations in low-density shells or deflagrations.",
"doi": "10.3847/1538-4357/abb45c",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-12-10",
"series_number": "1",
"volume": "905",
"issue": "1",
"pages": "Art. No. 58"
},
{
"id": "authors:8p1gs-8k497",
"collection": "authors",
"collection_id": "8p1gs-8k497",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200901-074328291",
"type": "article",
"title": "Constraining the Kilonova Rate with Zwicky Transient Facility Searches Independent of Gravitational Wave and Short Gamma-Ray Burst Triggers",
"author": [
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Sagu\u00e9s Carracedo",
"given_name": "Ana",
"clpid": "Sagu\u00e9s-Carracedo-Ana"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127",
"clpid": "Bulla-Mattia"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumada-Tom\u00e1s"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-Michael-W"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996",
"clpid": "Goobar-Ariel"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881",
"clpid": "Kaplan-David-L"
},
{
"family_name": "Loveridge",
"given_name": "Tegan T.",
"clpid": "Loveridge-Tegan-T"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Cooke",
"given_name": "Jeff",
"orcid": "0000-0001-5703-2108",
"clpid": "Cooke-Jeffrey"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-Ashot"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-Bradley"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Delacroix",
"given_name": "Alexandre",
"clpid": "Delacroix-Alexandre"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Zach"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-David-D-S"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-Thomas"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Smith",
"given_name": "Roger M.",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "Van Sistine",
"given_name": "Angela",
"orcid": "0000-0003-4131-173X",
"clpid": "Van-Sistine-Angela"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
}
],
"abstract": "The first binary neutron star merger, GW170817, was accompanied by a radioactivity-powered optical/infrared transient called a kilonova. To date, no compelling kilonova has been found in all-sky optical surveys, independently of short gamma-ray burst and gravitational-wave triggers. In this work, we searched the first 23 months of the Zwicky Transient Facility (ZTF) data stream for candidate kilonovae in the form of rapidly evolving transients. We combined ZTF alert queries with forced point-spread-function photometry and nightly flux stacking to increase our sensitivity to faint and fast transients. Automatic queries yielded >11,200 candidates, 24 of which passed quality checks and selection criteria based on a grid of kilonova models tailored for both binary neutron star and neutron star\u2013black hole mergers. None of the candidates in our sample was deemed a possible kilonova after thorough vetting. The sources that passed our selection criteria are dominated by Galactic cataclysmic variables. We identified two fast transients at high Galactic latitude, one of which is the confirmed afterglow of long-duration GRB 190106A, the other is a possible cosmological afterglow. Using a survey simulation code, we constrained the kilonova rate for a range of models including top-hat, linearly decaying light curves, and synthetic light curves obtained with radiative transfer simulations. For prototypical GW170817-like kilonovae, we constrain the rate to be R < 1775 Gpc\u207b\u00b3 yr\u207b\u00b9 (95% confidence). By assuming a population of kilonovae with the same geometry and composition of GW170817 observed under a uniform viewing angle distribution, we obtained a constraint on the rate of R < 4029 Gpc\u207b\u00b3 yr\u207b\u00b9.",
"doi": "10.3847/1538-4357/abbf4c",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-12-01",
"series_number": "2",
"volume": "904",
"issue": "2",
"pages": "Art. No. 155"
},
{
"id": "authors:yj29e-jv515",
"collection": "authors",
"collection_id": "yj29e-jv515",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200710-130233427",
"type": "article",
"title": "Age Dependence of Mid-infrared Emission around Young Star Clusters",
"author": [
{
"family_name": "Lin",
"given_name": "Zesen",
"orcid": "0000-0001-8078-3428",
"clpid": "Lin-Zesen"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Kong",
"given_name": "Xu",
"orcid": "0000-0002-7660-2273",
"clpid": "Kong-Xu"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Cignoni",
"given_name": "M.",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-M"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-K"
},
{
"family_name": "Grebel",
"given_name": "E. K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-E-K"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Sacchi",
"given_name": "E.",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-E"
},
{
"family_name": "Smith",
"given_name": "L. J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-L-J"
}
],
"abstract": "Using the star cluster catalogs from the Hubble Space Telescope program Legacy Extragalactic UV survey (LEGUS) and 8 \u03bcm images from the IRAC camera on the Spitzer Space Telescope for five galaxies within 5 Mpc, we investigate how the 8 \u03bcm dust luminosity correlates with the stellar age on the 30\u201350 pc scale of star-forming regions. We construct a sample of 97 regions centered at local peaks of 8 \u03bcm emission, each containing one or more young star cluster candidates from the LEGUS catalogs. We find a tight anticorrelation with a Pearson correlation coefficient of r = \u22120.84 \u00b1 0.05 between the mass-normalized dust-only 8 \u03bcm luminosity and the age of stellar clusters younger than 1 Gyr; the 8 \u03bcm luminosity decreases with increasing age of the stellar population. Simple assumptions on a combination of stellar and dust emission models reproduce the observed trend. We also explore how the scatter of the observed trend depends on assumptions of stellar metallicity, polycyclic aromatic hydrocarbon (PAH) abundance, fraction of stellar light absorbed by dust, and instantaneous versus continuous star formation models. We find that variations in stellar metallicity have little effect on the scatter, while PAH abundance and the fraction of dust-absorbed light bracket the full range of the data. We also find that the trend is better explained by continuous star formation, rather than instantaneous burst models. We ascribe this result to the presence of multiple star clusters with different ages in many of the regions. Upper limits of the dust-only 8 \u03bcm emission as a function of age are provided.",
"doi": "10.3847/1538-4357/ab9106",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-06-10",
"series_number": "1",
"volume": "896",
"issue": "1",
"pages": "Art. No. 16"
},
{
"id": "authors:t228f-t9m83",
"collection": "authors",
"collection_id": "t228f-t9m83",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191120-134817021",
"type": "article",
"title": "GROWTH on S190814bv: Deep Synoptic Limits on the Optical/Near-Infrared Counterpart to a Neutron Star-Black Hole Merger",
"author": [
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-J-E"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj R.",
"clpid": "Karambelkar-V-R"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Fremling",
"given_name": "U. Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-A"
},
{
"family_name": "Dahiwale",
"given_name": "Aishwarya",
"clpid": "Dahiwale-A-S"
},
{
"family_name": "Hankins",
"given_name": "Matthew",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-M-J"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-A"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
}
],
"abstract": "On 2019 August 14, the Advanced LIGO and Virgo interferometers detected the high-significance gravitational wave (GW) signal S190814bv. The GW data indicated that the event resulted from a neutron star\u2013black hole (NSBH) merger, or potentially a low-mass binary BH merger. Due to the low false-alarm rate and the precise localization (23 deg2 at 90%), S190814bv presented the community with the best opportunity yet to directly observe an optical/near-infrared counterpart to an NSBH merger. To search for potential counterparts, the GROWTH Collaboration performed real-time image subtraction on six nights of public Dark Energy Camera images acquired in the 3 weeks following the merger, covering >98% of the localization probability. Using a worldwide network of follow-up facilities, we systematically undertook spectroscopy and imaging of optical counterpart candidates. Combining these data with a photometric redshift catalog, we ruled out each candidate as the counterpart to S190814bv and placed deep, uniform limits on the optical emission associated with S190814bv. For the nearest consistent GW distance, radiative transfer simulations of NSBH mergers constrain the ejecta mass of S190814bv to be M_(ej) < 0.04 M\u2299 at polar viewing angles, or M_(ej) < 0.03 M\u2299 if the opacity is \u03ba < 2 cm\u00b2g\u207b\u00b9. Assuming a tidal deformability for the NS at the high end of the range compatible with GW170817 results, our limits would constrain the BH spin component aligned with the orbital momentum to be \u03c7 < 0.7 for mass ratios Q < 6, with weaker constraints for more compact NSs.",
"doi": "10.3847/1538-4357/ab6a1b",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-02-20",
"series_number": "2",
"volume": "890",
"issue": "2",
"pages": "Art. No. 131"
},
{
"id": "authors:ety11-1jm35",
"collection": "authors",
"collection_id": "ety11-1jm35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200624-104211145",
"type": "article",
"title": "LEGUS and H_\u03b1-LEGUS Observations of Star Clusters in NGC 4449: Improved Ages and the Fraction of Light in Clusters as a Function of Age",
"author": [
{
"family_name": "Whitmore",
"given_name": "Bradley C.",
"orcid": "0000-0002-3784-7032",
"clpid": "Whitmore-Bradley-C"
},
{
"family_name": "Chandar",
"given_name": "Rupali",
"orcid": "0000-0003-0085-4623",
"clpid": "Chandar-Rupali"
},
{
"family_name": "Lee",
"given_name": "Janice",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Ubeda",
"given_name": "Leonardo",
"clpid": "Ubeda-L"
},
{
"family_name": "Adamo",
"given_name": "Angela",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Aloisi",
"given_name": "Alessandra",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-A"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Cignoni",
"given_name": "Michele",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-M"
},
{
"family_name": "Cook",
"given_name": "David",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "Daniel",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Elmegreen",
"given_name": "B. G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-B-G"
},
{
"family_name": "Gouliermis",
"given_name": "Dimitrios",
"orcid": "0000-0002-2763-0075",
"clpid": "Gouliermis-D-A"
},
{
"family_name": "Grebel",
"given_name": "Eva K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-E-K"
},
{
"family_name": "Grasha",
"given_name": "Kathryn",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-K"
},
{
"family_name": "Johnson",
"given_name": "Kelsey E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-K-E"
},
{
"family_name": "Kim",
"given_name": "Hwihyun",
"orcid": "0000-0003-4770-688X",
"clpid": "Kim-Hwihyun"
},
{
"family_name": "Sacchi",
"given_name": "Elena",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-E"
},
{
"family_name": "Smith",
"given_name": "Linda J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-Linda-J"
},
{
"family_name": "Tosi",
"given_name": "Monica",
"orcid": "0000-0002-0986-4759",
"clpid": "Tosi-Monica"
},
{
"family_name": "Wofford",
"given_name": "Aida",
"orcid": "0000-0001-8289-3428",
"clpid": "Wofford-A"
}
],
"abstract": "We present a new catalog and results for the cluster system of the starburst galaxy NGC 4449, based on multiband imaging observations taken as part of the LEGUS and H_\u03b1-LEGUS surveys. We improve the spectral energy fitting method used to estimate cluster ages, and find that the results, particularly for older clusters, are in better agreement with those from spectroscopy. The inclusion of H_\u03b1 measurements, the role of stochasticity for low-mass clusters, the assumptions about reddening, and the choices of SSP model and metallicity all have important impacts on the age dating of clusters. A comparison with ages derived from stellar color\u2013magnitude diagrams for partially resolved clusters shows reasonable agreement, but large scatter in some cases. The fraction of light found in clusters relative to the total light (i.e., T_L) in the U, B, and V filters in 25 different \u2248 kiloparsec-size regions throughout NGC 4449 correlates with both the specific region luminosity, R_L , and the dominant age of the underlying stellar population in each region. The observed cluster age distribution is found to decline over time as dN/d\u03c4 \u221d \u03c4^\u03b3 , with \u03b3 = \u22120.85 \u00b1 0.15, independent of cluster mass, and is consistent with strong, early cluster disruption. The mass functions of the clusters can be described by a power law with dN/dM \u221d M^\u03b2 and \u03b2 = \u22121.86 \u00b1 0.2, independent of cluster age. The mass and age distributions are quite resilient to differences in age-dating methods. There is tentative evidence for a factor of 2\u20133 enhancement in both the star and cluster formation rate \u2248100\u2013300 Myr ago, indicating that cluster formation tracks star formation generally. The enhancement is probably associated with an earlier interaction event.",
"doi": "10.3847/1538-4357/ab59e5",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-02-01",
"series_number": "2",
"volume": "889",
"issue": "2",
"pages": "Art. No. 154"
},
{
"id": "authors:twnzd-gbz48",
"collection": "authors",
"collection_id": "twnzd-gbz48",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200113-112218745",
"type": "article",
"title": "Star-forming Clumps in Local Luminous Infrared Galaxies",
"author": [
{
"family_name": "Larson",
"given_name": "K. L.",
"orcid": "0000-0003-3917-6460",
"clpid": "Larson-K-L"
},
{
"family_name": "D\u00edaz-Santos",
"given_name": "T.",
"orcid": "0000-0003-0699-6083",
"clpid": "D\u00edaz-Santos-T"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Privon",
"given_name": "G. C.",
"orcid": "0000-0003-3474-1125",
"clpid": "Privon-G-C"
},
{
"family_name": "Linden",
"given_name": "S. T.",
"orcid": "0000-0002-1000-6081",
"clpid": "Linden-S-T"
},
{
"family_name": "Evans",
"given_name": "A. S.",
"orcid": "0000-0003-2638-1334",
"clpid": "Evans-A-S"
},
{
"family_name": "Howell",
"given_name": "J.",
"clpid": "Howell-J-H"
},
{
"family_name": "Charmandaris",
"given_name": "V.",
"orcid": "0000-0002-2688-1956",
"clpid": "Charmandaris-V"
},
{
"family_name": "U",
"given_name": "V.",
"orcid": "0000-0002-1912-0024",
"clpid": "U-Vivian"
},
{
"family_name": "Sanders",
"given_name": "D. B.",
"orcid": "0000-0002-1233-9998",
"clpid": "Sanders-D-B"
},
{
"family_name": "Stierwalt",
"given_name": "S.",
"orcid": "0000-0002-2596-8531",
"clpid": "Stierwalt-S"
},
{
"family_name": "Barcos-Mu\u00f1oz",
"given_name": "L.",
"orcid": "0000-0003-0057-8892",
"clpid": "Barcos-Mu\u00f1oz-L"
},
{
"family_name": "Rich",
"given_name": "J.",
"orcid": "0000-0002-5807-5078",
"clpid": "Rich-J-A"
},
{
"family_name": "Medling",
"given_name": "A.",
"orcid": "0000-0001-7421-2944",
"clpid": "Medling-A-M"
},
{
"family_name": "Cook",
"given_name": "D.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Oklop\u010di\u0107",
"given_name": "A.",
"orcid": "0000-0002-9584-6476",
"clpid": "Oklop\u010di\u0107-A"
},
{
"family_name": "Murphy",
"given_name": "E. J.",
"orcid": "0000-0001-7089-7325",
"clpid": "Murphy-E-J"
},
{
"family_name": "Bonfini",
"given_name": "P.",
"clpid": "Bonfini-P"
}
],
"abstract": "We present HST narrowband near-infrared imaging of Pa\u03b1 and Pa\u03b2 emission of 48 local luminous infrared galaxies (LIRGs) from the Great Observatories All-Sky LIRG Survey. These data allow us to measure the properties of 810 spatially resolved star-forming regions (59 nuclei and 751 extranuclear clumps) and directly compare their properties to those found in both local and high-redshift star-forming galaxies. We find that in LIRGs the star-forming clumps have radii ranging from ~90 to 900 pc and star formation rates (SFRs) of ~1 \u00d7 10\u207b\u00b3 to 10 M\u2299 yr\u207b\u00b9, with median values for extranuclear clumps of 170 pc and 0.03 M\u2299 yr\u207b\u00b9. The detected star-forming clumps are young, with a median stellar age of 8.7 Myr, and have a median stellar mass of 5 \u00d7 10\u2075 M \u2299. The SFRs span the range of those found in normal local star-forming galaxies to those found in high-redshift star-forming galaxies at z = 1\u20133. The luminosity function of the LIRG clumps has a flatter slope than found in lower-luminosity, star-forming galaxies, indicating a relative excess of luminous star-forming clumps. In order to predict the possible range of star-forming histories and gas fractions, we compare the star-forming clumps to those measured in the MassiveFIRE high-resolution cosmological simulation. The star-forming clumps in MassiveFIRE cover the same range of SFRs and sizes found in the local LIRGs and have total gas fractions that extend from 10% to 90%. If local LIRGs are similar to these simulated galaxies, we expect that future observations with ALMA will find a large range of gas fractions, and corresponding star formation efficiencies, among the star-forming clumps in LIRGs.",
"doi": "10.3847/1538-4357/ab5dc3",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-01-10",
"series_number": "2",
"volume": "888",
"issue": "2",
"pages": "Art. No. 92"
},
{
"id": "authors:atgr9-w1d26",
"collection": "authors",
"collection_id": "atgr9-w1d26",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200402-090152205",
"type": "article",
"title": "Spatial Segregation of Massive Clusters in Dwarf Galaxies",
"author": [
{
"family_name": "Elmegreen",
"given_name": "Bruce G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-B-G"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176",
"clpid": "Boquien-M"
},
{
"family_name": "Bournaud",
"given_name": "F.",
"orcid": "0000-0002-5743-0250",
"clpid": "Bournaud-F"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Duc",
"given_name": "P.-A.",
"clpid": "Duc-P-A"
},
{
"family_name": "Elmegreen",
"given_name": "D. M.",
"orcid": "0000-0002-1392-3520",
"clpid": "Elmegreen-D-M"
},
{
"family_name": "Fensch",
"given_name": "J.",
"orcid": "0000-0002-4383-0202",
"clpid": "Fensch-J"
},
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-K"
},
{
"family_name": "Kim",
"given_name": "Hwi",
"orcid": "0000-0003-4770-688X",
"clpid": "Kim-Hwihyun"
},
{
"family_name": "Kahre",
"given_name": "L.",
"orcid": "0000-0002-2037-3096",
"clpid": "Kahre-L"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Ryon",
"given_name": "J. E.",
"clpid": "Ryon-J-E"
},
{
"family_name": "Sabbi",
"given_name": "E.",
"orcid": "0000-0003-2954-7643",
"clpid": "Sabbi-E"
},
{
"family_name": "Smith",
"given_name": "L. J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-L-J"
}
],
"abstract": "The relative average minimum projected separations of star clusters in the Legacy ExtraGalactic UV Survey (LEGUS) and in tidal dwarfs around the interacting galaxy NGC 5291 are determined as a function of cluster mass to look for cluster\u2013cluster mass segregation. Class 2 and 3 LEGUS clusters, which have a more irregular internal structure than the compact and symmetric class 1 clusters, are found to be mass-segregated in low-mass galaxies, which means that the more massive clusters are systematically bunched together compared to the lower-mass clusters. This mass segregation is not present in high-mass galaxies or class 1 clusters. We consider possible causes for this segregation, including differences in cluster formation and scattering in the shallow gravitational potentials of low-mass galaxies.",
"doi": "10.3847/2041-8213/ab632a",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2020-01-10",
"series_number": "2",
"volume": "888",
"issue": "2",
"pages": "Art. No. L27"
},
{
"id": "authors:tscqj-2mx78",
"collection": "authors",
"collection_id": "tscqj-2mx78",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200131-123803370",
"type": "article",
"title": "Star Formation Histories of the LEGUS Dwarf Galaxies. III. The Nonbursty Nature of 23 Star-forming Dwarf Galaxies",
"author": [
{
"family_name": "Cignoni",
"given_name": "M.",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-M"
},
{
"family_name": "Sacchi",
"given_name": "E.",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-E"
},
{
"family_name": "Tosi",
"given_name": "M.",
"orcid": "0000-0002-0986-4759",
"clpid": "Tosi-M"
},
{
"family_name": "Aloisi",
"given_name": "A.",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-A"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Lee",
"given_name": "J. C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Sabbi",
"given_name": "E.",
"orcid": "0000-0003-2954-7643",
"clpid": "Sabbi-E"
},
{
"family_name": "Thilker",
"given_name": "D. A.",
"orcid": "0000-0002-8528-7340",
"clpid": "Thilker-D-A"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Elmegreen",
"given_name": "B. G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-B-G"
},
{
"family_name": "Gallagher",
"given_name": "J. S., III",
"orcid": "0000-0001-8608-0408",
"clpid": "Gallagher-J-S-III"
},
{
"family_name": "Grebel",
"given_name": "E. K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-E-K"
},
{
"family_name": "Johnson",
"given_name": "K. E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-K-E"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Smith",
"given_name": "L. J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-L-J"
},
{
"family_name": "Ubeda",
"given_name": "L.",
"clpid": "Ubeda-L"
}
],
"abstract": "We derive the recent star formation histories (SFHs) of 23 active dwarf galaxies using Hubble Space Telescope observations from the Legacy Extragalactic UV Survey. We apply a color\u2013magnitude diagram (CMD) fitting technique using two independent sets of stellar models, PARSEC-COLIBRI and MIST. Despite the nonnegligible recent activity, none of the 23 star-forming dwarfs show enhancements in the last 100 Myr larger than three times the 100 Myr average. The unweighted mean of the individual SFHs in the last 100 Myr is also consistent with a rather constant activity, irrespective of the atomic gas fraction. We confirm previous results that for dwarf galaxies, the CMD-based average star formation rates (SFRs) are generally higher than the FUV-based SFRs. For half of the sample, the 60 Myr average CMD-based SFR is more than two times the FUV SFR. In contrast, we find remarkable agreement between the 10 Myr average CMD-based SFR and the H\u03b1-based SFR. Finally, using core helium-burning stars of intermediate mass, we study the pattern of star formation spatial progression over the past 60 Myr and speculate on the possible triggers and connections of the star formation activity with the environment in which these galaxies live. Approximately half of our galaxies show spatial progression of star formation in the last 60 Myr and/or very recent diffuse and off-center activity compared to RGB stars.",
"doi": "10.3847/1538-4357/ab53d5",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-12-20",
"series_number": "2",
"volume": "887",
"issue": "2",
"pages": "Art. No. 112"
},
{
"id": "authors:2tpjf-30z54",
"collection": "authors",
"collection_id": "2tpjf-30z54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200110-093456510",
"type": "article",
"title": "H\u00a0\u03b1 morphologies of star clusters: a LEGUS study of H\u00a0II region evolution time-scales and stochasticity in low-mass clusters",
"author": [
{
"family_name": "Hannon",
"given_name": "Stephen",
"orcid": "0000-0001-9628-8958",
"clpid": "Hannon-Stephen"
},
{
"family_name": "Lee",
"given_name": "Janice C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Whitmore",
"given_name": "B. C.",
"orcid": "0000-0002-3784-7032",
"clpid": "Whitmore-B-C"
},
{
"family_name": "Chandar",
"given_name": "R.",
"clpid": "Chandar-R"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Mobasher",
"given_name": "B.",
"clpid": "Mobasher-Bahram"
},
{
"family_name": "Aloisi",
"given_name": "A.",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-Alessandra"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-Daniela"
},
{
"family_name": "Cignoni",
"given_name": "M.",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-Michele"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "D.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-Daniel-A"
},
{
"family_name": "Deger",
"given_name": "S.",
"orcid": "0000-0003-1943-723X",
"clpid": "Deger-Sinan"
},
{
"family_name": "Della Bruna",
"given_name": "L.",
"clpid": "Della-Bruna-L"
},
{
"family_name": "Elmegreen",
"given_name": "D. M.",
"orcid": "0000-0002-1392-3520",
"clpid": "Elmegreen-Debra-M"
},
{
"family_name": "Gouliermis",
"given_name": "D. A.",
"orcid": "0000-0002-2763-0075",
"clpid": "Gouliermis-Dimitrios-A"
},
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-Kathryn"
},
{
"family_name": "Grebel",
"given_name": "E. K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-Eva-K"
},
{
"family_name": "Herrero",
"given_name": "A.",
"orcid": "0000-0001-8768-2179",
"clpid": "Herrero-Artemio"
},
{
"family_name": "Hunter",
"given_name": "D. A.",
"orcid": "0000-0002-3322-9798",
"clpid": "Hunter-Deidre-A"
},
{
"family_name": "Johnson",
"given_name": "K. E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-Kelsey-E"
},
{
"family_name": "Kennicutt",
"given_name": "R.",
"orcid": "0000-0001-5448-1821",
"clpid": "Kennicutt-Robert-C"
},
{
"family_name": "Kim",
"given_name": "H.",
"clpid": "Kim-H"
},
{
"family_name": "Sacchi",
"given_name": "E.",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-Elena"
},
{
"family_name": "Smith",
"given_name": "L.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-Linda-J"
},
{
"family_name": "Thilker",
"given_name": "D.",
"orcid": "0000-0002-8528-7340",
"clpid": "Thilker-David-A"
},
{
"family_name": "Turner",
"given_name": "J.",
"clpid": "Turner-J"
},
{
"family_name": "Walterbos",
"given_name": "R. A. M.",
"clpid": "Walterbos-R-A-M"
},
{
"family_name": "Wofford",
"given_name": "A.",
"clpid": "Wofford-A"
}
],
"abstract": "The morphology of H II regions around young star clusters provides insight into the time-scales and physical processes that clear a cluster's natal gas. We study \u223c700 young clusters (\u226410\u2009Myr) in three nearby spiral galaxies (NGC 7793, NGC 4395, and NGC 1313) using Hubble Space Telescope (HST) imaging from LEGUS (Legacy ExtraGalactic Ultraviolet Survey). Clusters are classified by their H \u03b1 morphology (concentrated, partially exposed, no-emission) and whether they have neighbouring clusters (which could affect the clearing time-scales). Through visual inspection of the HST images, and analysis of ages, reddenings, and stellar masses from spectral energy distributions fitting, together with the (U\u2212 B), (V \u2212 I) colours, we find (1) the median ages indicate a progression from concentrated (\u223c3\u2009Myr), to partially exposed (\u223c4\u2009Myr), to no H \u03b1 emission (>5\u2009Myr), consistent with the expected temporal evolution of H II regions and previous results. However, (2) similarities in the age distributions for clusters with concentrated and partially exposed H \u03b1 morphologies imply a short time-scale for gas clearing (\u22721\u2009Myr). Also, (3) our cluster sample's median mass is \u223c1000 M\u2299, and a significant fraction (\u223c20 per cent\u2060) contain one or more bright red sources (presumably supergiants), which can mimic reddening effects. Finally, (4) the median E(B \u2212 V) values for clusters with concentrated H \u03b1 and those without H \u03b1 emission appear to be more similar than expected (\u223c0.18 versus \u223c0.14, respectively), but when accounting for stochastic effects, clusters without H \u03b1 emission are less reddened. To mitigate stochastic effects, we experiment with synthesizing more massive clusters by stacking fluxes of clusters within each H \u03b1 morphological class. Composite isolated clusters also reveal a colour and age progression for H \u03b1 morphological classes, consistent with analysis of the individual clusters.",
"doi": "10.1093/mnras/stz2820",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2019-12",
"series_number": "4",
"volume": "490",
"issue": "4",
"pages": "4648-4665"
},
{
"id": "authors:bbnt6-sag19",
"collection": "authors",
"collection_id": "bbnt6-sag19",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190802-094555948",
"type": "article",
"title": "GROWTH on S190425z: Searching Thousands of Square Degrees to Identify an Optical or Infrared Counterpart to a Binary Neutron Star Merger with the Zwicky Transient Facility and Palomar Gattini-IR",
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"family_name": "Coughlin",
"given_name": "Michael W.",
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{
"family_name": "Anand",
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{
"family_name": "De",
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{
"family_name": "Hankins",
"given_name": "Matthew J.",
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{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
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{
"family_name": "Singer",
"given_name": "Leo P.",
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{
"family_name": "Bellm",
"given_name": "Eric C.",
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{
"family_name": "Andreoni",
"given_name": "Igor",
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{
"family_name": "Cenko",
"given_name": "S. Bradley",
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"family_name": "Dugas",
"given_name": "Alison M.",
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"family_name": "Jencson",
"given_name": "Jacob E.",
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{
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{
"family_name": "Dekany",
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{
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{
"family_name": "Duev",
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{
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{
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{
"family_name": "Goldstein",
"given_name": "Daniel A.",
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{
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{
"family_name": "Goobar",
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{
"family_name": "Graham",
"given_name": "Matthew J.",
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{
"family_name": "Hanayama",
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{
"family_name": "Horiuchi",
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{
"family_name": "Hung",
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{
"family_name": "Jha",
"given_name": "Saurabh W.",
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{
"family_name": "Kong",
"given_name": "Albert K. H.",
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{
"family_name": "Giomi",
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{
"family_name": "Kaplan",
"given_name": "David L.",
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{
"family_name": "Karambelkar",
"given_name": "V. R.",
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{
"family_name": "Kowalski",
"given_name": "Marek",
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{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
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{
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{
"family_name": "Masci",
"given_name": "Frank J.",
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{
"family_name": "Mazzali",
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{
"family_name": "Moore",
"given_name": "Anna M.",
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{
"family_name": "Mogotsi",
"given_name": "Moses",
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{
"family_name": "Neill",
"given_name": "James D.",
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"clpid": "Neill-J-D"
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{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554",
"clpid": "Ngeow-Chow-Choong"
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{
"family_name": "Mart\u00ednez-Palomera",
"given_name": "Jorge",
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"clpid": "Mart\u00ednez-Palomera-J"
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{
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"given_name": "Valentina",
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{
"family_name": "Pavana",
"given_name": "M.",
"orcid": "0000-0002-0000-1543",
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{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774",
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{
"family_name": "Patil",
"given_name": "Atharva Sunil",
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{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
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{
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{
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{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
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{
"family_name": "Sharma",
"given_name": "Yashvi",
"clpid": "Sharma-Y"
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{
"family_name": "Singh",
"given_name": "Avinash",
"clpid": "Singh-Avinash"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-J"
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{
"family_name": "Soon",
"given_name": "Jamie",
"clpid": "Soon-Jamie"
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{
"family_name": "Staats",
"given_name": "Kai",
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{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558",
"clpid": "Taggart-K"
},
{
"family_name": "Tan",
"given_name": "Hanjie",
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{
"family_name": "Travouillon",
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{
"family_name": "Troja",
"given_name": "Eleonora",
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{
"family_name": "Waratkar",
"given_name": "Gaurav",
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"clpid": "Waratkar-G"
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{
"family_name": "Yatsu",
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],
"abstract": "The third observing run by LVC has brought the discovery of many compact binary coalescences. Following the detection of the first binary neutron star merger in this run (LIGO/Virgo S190425z), we performed a dedicated follow-up campaign with the Zwicky Transient Facility (ZTF) and Palomar Gattini-IR telescopes. The initial skymap of this single-detector gravitational wave (GW) trigger spanned most of the sky observable from Palomar Observatory. Covering 8000 deg\u00b2 of the initial skymap over the next two nights, corresponding to 46% integrated probability, ZTF system achieved a depth of \u224821 m_(AB) in g- and r-bands. Palomar Gattini-IR covered 2200 square degrees in J-band to a depth of 15.5 mag, including 32% integrated probability based on the initial skymap. The revised skymap issued the following day reduced these numbers to 21% for the ZTF and 19% for Palomar Gattini-IR. We narrowed 338,646 ZTF transient \"alerts\" over the first two nights of observations to 15 candidate counterparts. Two candidates, ZTF19aarykkb and ZTF19aarzaod, were particularly compelling given that their location, distance, and age were consistent with the GW event, and their early optical light curves were photometrically consistent with that of kilonovae. These two candidates were spectroscopically classified as young core-collapse supernovae. The remaining candidates were ruled out as supernovae. Palomar Gattini-IR did not identify any viable candidates with multiple detections only after merger time. We demonstrate that even with single-detector GW events localized to thousands of square degrees, systematic kilonova discovery is feasible.",
"doi": "10.3847/2041-8213/ab4ad8",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-11-01",
"series_number": "1",
"volume": "885",
"issue": "1",
"pages": "Art. No. L19"
},
{
"id": "authors:tr1t6-kgt55",
"collection": "authors",
"collection_id": "tr1t6-kgt55",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190619-081420386",
"type": "article",
"title": "GROWTH on S190510g: DECam Observation Planning and Follow-Up of a Distant Binary Neutron Star Merger Candidate",
"author": [
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597",
"clpid": "Singer-L-P"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumada-T"
},
{
"family_name": "Medford",
"given_name": "Michael",
"orcid": "0000-0002-7226-0659",
"clpid": "Medford-M"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-E-C"
},
{
"family_name": "Webb",
"given_name": "Sara",
"orcid": "0000-0003-2601-1472",
"clpid": "Webb-S"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127",
"clpid": "Bulla-M"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X",
"clpid": "Bloom-J-S"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Nugent",
"given_name": "Peter E.",
"orcid": "0000-0002-3389-0586",
"clpid": "Nugent-P-E"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-A"
},
{
"family_name": "Barnes",
"given_name": "Jennifer",
"orcid": "0000-0003-3340-4784",
"clpid": "Barnes-J"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Cooke",
"given_name": "Jeff",
"orcid": "0000-0001-5703-2108",
"clpid": "Cooke-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Fremling",
"given_name": "U. Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230",
"clpid": "Gatkine-P"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Z"
},
{
"family_name": "Kong",
"given_name": "Albert K. H.",
"orcid": "0000-0002-5105-344X",
"clpid": "Kong-Albert-K-H"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Mart\u00ednez-Palomera",
"given_name": "Jorge",
"orcid": "0000-0002-7395-4935",
"clpid": "Mart\u00ednez-Palomera-J"
},
{
"family_name": "Tao",
"given_name": "Duo",
"clpid": "Tao-Duo"
},
{
"family_name": "Zhang",
"given_name": "Keming",
"orcid": "0000-0002-9870-5695",
"clpid": "Zhang-Keming"
}
],
"abstract": "The first two months of the third Advanced LIGO and Virgo observing run (2019 April\u2013May) showed that distant gravitational-wave (GW) events can now be readily detected. Three candidate mergers containing neutron stars (NS) were reported in a span of 15 days, all likely located more than 100 Mpc away. However, distant events such as the three new NS mergers are likely to be coarsely localized, which highlights the importance of facilities and scheduling systems that enable deep observations over hundreds to thousands of square degrees to detect the electromagnetic counterparts. On 2019 May 10 02:59:39.292 UT the GW candidate S190510g was discovered and initially classified as a binary neutron star (BNS) merger with 98% probability. The GW event was localized within an area of 3462 deg^2, later refined to 1166 deg^2 (90%) at a distance of 227 \u00b1 92 Mpc. We triggered Target-of-Opportunity observations with the Dark Energy Camera (DECam), a wide-field optical imager mounted at the prime focus of the 4 m Blanco Telescope at Cerro Tololo Inter-American Observatory in Chile. This Letter describes our DECam observations and our real-time analysis results, focusing in particular on the design and implementation of the observing strategy. Within 24 hr of the merger time, we observed 65% of the total enclosed probability of the final skymap with an observing efficiency of 94%. We identified and publicly announced 13 candidate counterparts. S190510g was reclassified 1.7 days after the merger, after our observations were completed, with a \"BNS merger\" probability reduced from 98% to 42% in favor of a \"terrestrial classification.",
"doi": "10.3847/2041-8213/ab3399",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-08-10",
"series_number": "1",
"volume": "881",
"issue": "1",
"pages": "Art. No. L16"
},
{
"id": "authors:43bjy-4dr06",
"collection": "authors",
"collection_id": "43bjy-4dr06",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190107-091211377",
"type": "article",
"title": "Census of the Local Universe (CLU) Narrowband Survey. I. Galaxy Catalogs from Preliminary Fields",
"author": [
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Van Sistine",
"given_name": "Angela",
"orcid": "0000-0003-4131-173X",
"clpid": "Van-Sistine-A"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881",
"clpid": "Kaplan-D-L"
},
{
"family_name": "Sutter",
"given_name": "Jessica S.",
"orcid": "0000-0002-9183-8102",
"clpid": "Sutter-J-S"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Dale",
"given_name": "Daniel A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Sesar",
"given_name": "Branimir",
"orcid": "0000-0002-0834-3978",
"clpid": "Sesar-B"
},
{
"family_name": "Brady",
"given_name": "Patrick R.",
"orcid": "0000-0002-4611-9387",
"clpid": "Brady-P-R"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774",
"clpid": "Ofek-E-O"
},
{
"family_name": "Reitze",
"given_name": "David H.",
"clpid": "Reitze-D-H"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "We present the Census of the Local Universe (CLU) narrowband survey to search for emission-line (H\u03b1) galaxies. CLU-H\u03b1 has imaged \u22483\u03c0 of the sky (26,470 deg^2) with four narrowband filters that probe a distance out to 200 Mpc. We have obtained spectroscopic follow-up for galaxy candidates in 14 preliminary fields (101.6 deg2) to characterize the limits and completeness of the survey. In these preliminary fields, CLU can identify emission lines down to an H\u03b1 flux limit of 10^(\u221214) erg s^(\u22121) cm^(\u22122) at 90% completeness, and recovers 83% (67%) of the H\u03b1 flux from cataloged galaxies in our search volume at the \u03a3 = 2.5 (\u03a3 = 5) color excess levels. The contamination from galaxies with no emission lines is 61% (12%) for \u03a3 = 2.5 (\u03a3 = 5). Also, in the regions of overlap between our preliminary fields and previous emission-line surveys, we recover the majority of the galaxies found in previous surveys and identify an additional \u2248300 galaxies. In total, we find 90 galaxies with no previous distance information, several of which are interesting objects: 7 blue compact dwarfs, 1 green pea, and a Seyfert galaxy; we also identify a known planetary nebula. These objects show that the CLU-H\u03b1 survey can be a discovery machine for objects in our own Galaxy and extreme galaxies out to intermediate redshifts. However, the majority of the CLU-H\u03b1 galaxies identified in this work show properties consistent with normal star-forming galaxies. CLU-H\u03b1 galaxies with new redshifts will be added to existing galaxy catalogs to focus the search for the electromagnetic counterpart to gravitational wave events.",
"doi": "10.3847/1538-4357/ab2131",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-07-20",
"series_number": "1",
"volume": "880",
"issue": "1",
"pages": "Art. No. 7"
},
{
"id": "authors:4eb3d-6mw74",
"collection": "authors",
"collection_id": "4eb3d-6mw74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190415-151755923",
"type": "article",
"title": "Star cluster catalogues for the LEGUS dwarf galaxies",
"author": [
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Martin",
"given_name": "C.",
"orcid": "0000-0002-8650-1644",
"clpid": "Martin-D-Christopher"
},
{
"family_name": "Lee",
"given_name": "J. C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Van Dyk",
"given_name": "S. D.",
"orcid": "0000-0001-9038-9950",
"clpid": "Van-Dyk-S-D"
}
],
"abstract": "We present the star cluster catalogues for 17 dwarf and irregular galaxies in the HST Treasury Program 'Legacy ExtraGalactic UV Survey' (LEGUS). Cluster identification and photometry in this sub-sample are similar to that of the entire LEGUS sample, but special methods were developed to provide robust catalogues with accurate fluxes due to low cluster statistics. The colours and ages are largely consistent for two widely used aperture corrections, but a significant fraction of the clusters are more compact than the average training cluster. However, the ensemble luminosity, mass, and age distributions are consistent suggesting that the systematics between the two methods are less than the random errors. When compared with the clusters from previous dwarf galaxy samples, we find that the LEGUS catalogues are more complete and provide more accurate total fluxes. Combining all clusters into a composite dwarf galaxy, we find that the luminosity and mass functions can be described by a power law with the canonical index of \u22122 independent of age and global SFR binning. The age distribution declines as a power law, with an index of \u2248\u2212 0.80 \u00b1 0.15, independent of cluster mass and global SFR binning. This decline of clusters is dominated by cluster disruption since the combined star formation histories and integrated-light SFRs are both approximately constant over the last few hundred Myr. Finally, we find little evidence for an upper-mass cut-off (< 2\u03c3) in the composite cluster mass function, and can rule out a truncation mass below \u224810^(4.5)M\u2299 but cannot rule out the existence of a truncation at higher masses.",
"doi": "10.1093/mnras/stz331",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2019-04",
"series_number": "4",
"volume": "484",
"issue": "4",
"pages": "4897-4919"
},
{
"id": "authors:ehyzk-5qm36",
"collection": "authors",
"collection_id": "ehyzk-5qm36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181129-112707921",
"type": "article",
"title": "Connecting young star clusters to CO molecular gas in NGC 7793 with ALMA\u2013LEGUS",
"author": [
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-K"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Bittle",
"given_name": "L.",
"clpid": "Bittle-L"
},
{
"family_name": "Johnson",
"given_name": "K. E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-K-E"
},
{
"family_name": "Donovan Meyer",
"given_name": "J.",
"orcid": "0000-0002-3106-7676",
"clpid": "Donovan-Meyer-J-L"
},
{
"family_name": "Kennicutt",
"given_name": "R. C.",
"orcid": "0000-0001-5448-1821",
"clpid": "Kennicutt-R-C"
},
{
"family_name": "Elmegreen",
"given_name": "B. G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-B-G"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Krumholz",
"given_name": "M. R.",
"orcid": "0000-0003-3893-854X",
"clpid": "Krumholz-M-R"
},
{
"family_name": "Fumagalli",
"given_name": "M.",
"orcid": "0000-0001-6676-3842",
"clpid": "Fumagalli-M"
},
{
"family_name": "Grebel",
"given_name": "E. K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-E-K"
},
{
"family_name": "Gouliermis",
"given_name": "D. A.",
"orcid": "0000-0002-2763-0075",
"clpid": "Gouliermis-D-A"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Gallagher",
"given_name": "J. S., III",
"orcid": "0000-0001-8608-0408",
"clpid": "Gallagher-J-S-III"
},
{
"family_name": "Aloisi",
"given_name": "A.",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-A"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Linden",
"given_name": "S.",
"orcid": "0000-0002-1000-6081",
"clpid": "Linden-S-T"
},
{
"family_name": "Sacchi",
"given_name": "E.",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-E"
},
{
"family_name": "Thilker",
"given_name": "D. A.",
"orcid": "0000-0002-8528-7340",
"clpid": "Thilker-D-A"
},
{
"family_name": "Walterbos",
"given_name": "R. A. M.",
"clpid": "Walterbos-R-A-M"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Wofford",
"given_name": "A.",
"clpid": "Wofford-A"
},
{
"family_name": "Smith",
"given_name": "L. J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-L-J"
}
],
"abstract": "We present an investigation of the relationship between giant molecular cloud (GMC) properties and the associated stellar clusters in the nearby flocculent galaxy NGC 7793. We combine the star cluster catalogue from the HST LEGUS (Legacy ExtraGalactic UV Survey) programme with the 15 pc resolution ALMA CO(2\u20131) observations. We find a strong spatial correlation between young star clusters and GMCs such that all clusters still associated with a GMC are younger than 11 Myr and display a median age of 2 Myr. The age distribution increases gradually as the cluster\u2013GMC distance increases, with star clusters that are spatially unassociated with molecular gas exhibiting a median age of 7 Myr. Thus, star clusters are able to emerge from their natal clouds long before the time-scale required for clouds to disperse. To investigate if the hierarchy observed in the stellar components is inherited from the GMCs, we quantify the amount of clustering in the spatial distributions of the components and find that the star clusters have a fractal dimension slope of \u22120.35 \u00b1 0.03, significantly more clustered than the molecular cloud hierarchy with slope of \u22120.18 \u00b1 0.04 over the range 40\u2013800 pc. We find, however, that the spatial clustering becomes comparable in strength for GMCs and star clusters with slopes of \u22120.44 \u00b1 0.03 and \u22120.45 \u00b1 0.06, respectively, when we compare massive (>10^5 M_\u2299) GMCs to massive and young star clusters. This shows that massive star clusters trace the same hierarchy as their parent GMCs, under the assumption that the star formation efficiency is a few per cent.",
"doi": "10.1093/mnras/sty2154",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2018-11-21",
"series_number": "1",
"volume": "481",
"issue": "1",
"pages": "1016-1027"
},
{
"id": "authors:xh063-2en23",
"collection": "authors",
"collection_id": "xh063-2en23",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180910-104151114",
"type": "article",
"title": "A UV resonance line echo from a shell around a hydrogen-poor superluminous supernova",
"author": [
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-R"
},
{
"family_name": "Fransson",
"given_name": "C.",
"orcid": "0000-0001-8532-3594",
"clpid": "Fransson-C"
},
{
"family_name": "Vreeswijk",
"given_name": "P. M.",
"orcid": "0000-0002-7572-9088",
"clpid": "Vreeswijk-P-M"
},
{
"family_name": "Woosley",
"given_name": "S. E.",
"clpid": "Woosley-S-E"
},
{
"family_name": "Leloudas",
"given_name": "G.",
"orcid": "0000-0002-8597-0756",
"clpid": "Leloudas-G"
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-D-A"
},
{
"family_name": "Quimby",
"given_name": "R. M.",
"orcid": "0000-0001-9171-5236",
"clpid": "Quimby-R-M"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Blagorodnova",
"given_name": "N.",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "Bue",
"given_name": "B. D.",
"orcid": "0000-0002-7856-3570",
"clpid": "Bue-B-D"
},
{
"family_name": "Cenko",
"given_name": "S. B.",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "De Cia",
"given_name": "A.",
"orcid": "0000-0003-2082-1626",
"clpid": "De-Cia-A"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Fremling",
"given_name": "C. U.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Gatkine",
"given_name": "P.",
"orcid": "0000-0002-1955-2230",
"clpid": "Gatkine-P"
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598",
"clpid": "Gal-Yam-A"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Nugent",
"given_name": "P. E.",
"orcid": "0000-0002-3389-0586",
"clpid": "Nugent-P-E"
},
{
"family_name": "Nyholm",
"given_name": "A.",
"clpid": "Nyholm-A"
},
{
"family_name": "Rubin",
"given_name": "A.",
"clpid": "Rubin-A-E"
},
{
"family_name": "Suzuki",
"given_name": "N.",
"clpid": "Suzuki-Naoyuki"
},
{
"family_name": "Wozniak",
"given_name": "P.",
"orcid": "0000-0002-9919-3310",
"clpid": "Wo\u017aniak-P-R"
}
],
"abstract": "Hydrogen-poor superluminous supernovae (SLSN-I) are a class of rare and energetic explosions that have been discovered in untargeted transient surveys in the past decade. The progenitor stars and the physical mechanism behind their large radiated energies (about 10^(51)\u2009erg or 10^(44)\u2009J) are both debated, with one class of models primarily requiring a large rotational energy and the other requiring very massive progenitors that either convert kinetic energy into radiation through interaction with circumstellar material (CSM) or engender an explosion caused by pair-instability (loss of photon pressure due to particle\u2013antiparticle production). Observing the structure of the CSM around SLSN-I offers a powerful test of some scenarios, although direct observations are scarce. Here, we present a series of spectroscopic observations of the SLSN-I iPTF16eh, which reveal both absorption and time- and frequency-variable emission in the Mg IIresonance doublet. We show that these observations are naturally explained as a resonance scattering light echo from a circumstellar shell. Modelling the evolution of the emission, we infer a shell radius of 0.1\u2009pc and velocity of 3,300\u2009km\u2009s\u22121, implying that the shell was ejected three decades before the supernova explosion. These properties match theoretical predictions of shell ejections occurring because of pulsational pair-instability and imply that the progenitor had a helium core mass of about 50\u201355 M_\u2299, corresponding to an initial mass of about 115 M_\u2299.",
"doi": "10.1038/s41550-018-0568-z",
"issn": "2397-3366",
"publisher": "Nature Publishing Group",
"publication": "Nature Astronomy",
"publication_date": "2018-11",
"series_number": "11",
"volume": "2",
"issue": "11",
"pages": "887-895"
},
{
"id": "authors:6ec90-4vd03",
"collection": "authors",
"collection_id": "6ec90-4vd03",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180620-135324765",
"type": "article",
"title": "A Comparison of Young Star Properties with Local Galactic Environment for LEGUS/LITTLE THINGS Dwarf Irregular Galaxies",
"author": [
{
"family_name": "Hunter",
"given_name": "Deidre A.",
"orcid": "0000-0002-3322-9798",
"clpid": "Hunter-D-A"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
}
],
"abstract": "We have explored the role environmental factors play in determining characteristics of young stellar objects in nearby dwarf irregular and blue compact dwarf galaxies. Star clusters are characterized by concentrations, masses, and formation rates; OB associations by mass and mass surface density; O stars by their numbers and near-ultraviolet absolute magnitudes; and H ii regions by H\u03b1 surface brightnesses. These characteristics are compared to surrounding galactic pressure, stellar mass density, H i surface density, and star formation rate (SFR) surface density. We find no trend of cluster characteristics with environmental properties, implying that larger-scale effects are more important in determining cluster characteristics or that rapid dynamical evolution erases any memory of the initial conditions. On the other hand, the most massive OB associations are found at higher pressure and H i surface density, and there is a trend of higher H ii region H\u03b1 surface brightness with higher pressure, suggesting that a higher concentration of massive stars and gas is found preferentially in regions of higher pressure. At low pressures we find massive stars but not bound clusters and OB associations. We do not find evidence for an increase of cluster formation efficiency as a function of SFR density. However, there is an increase in the ratio of the number of clusters to the number of O stars with increasing pressure, perhaps reflecting an increase in clustering properties with SFR.",
"doi": "10.3847/1538-3881/aac50e",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2018-07",
"series_number": "1",
"volume": "156",
"issue": "1",
"pages": "Art. No. 21"
},
{
"id": "authors:dd514-pjq24",
"collection": "authors",
"collection_id": "dd514-pjq24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180411-150615795",
"type": "article",
"title": "Star Formation Histories of the LEGUS Dwarf Galaxies. I. Recent History of NGC 1705, NGC 4449, and Holmberg II",
"author": [
{
"family_name": "Cignoni",
"given_name": "M.",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-M"
},
{
"family_name": "Sacchi",
"given_name": "E.",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-E"
},
{
"family_name": "Aloisi",
"given_name": "A.",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-A"
},
{
"family_name": "Tosi",
"given_name": "M.",
"orcid": "0000-0002-0986-4759",
"clpid": "Tosi-M"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Lee",
"given_name": "J. C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Sabbi",
"given_name": "E.",
"orcid": "0000-0003-2954-7643",
"clpid": "Sabbi-E"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Elmegreen",
"given_name": "B. G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-B-G"
},
{
"family_name": "Gallagher",
"given_name": "J. S., III",
"orcid": "0000-0001-8608-0408",
"clpid": "Gallagher-J-S-III"
},
{
"family_name": "Gouliermis",
"given_name": "D. A.",
"orcid": "0000-0002-2763-0075",
"clpid": "Gouliermis-D-A"
},
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-K"
},
{
"family_name": "Grebel",
"given_name": "E. K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-E-K"
},
{
"family_name": "Hunter",
"given_name": "D. A.",
"orcid": "0000-0002-3322-9798",
"clpid": "Hunter-D-A"
},
{
"family_name": "Johnson",
"given_name": "K. E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-K-E"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Smith",
"given_name": "L. J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-L-J"
},
{
"family_name": "Thilker",
"given_name": "D. A.",
"orcid": "0000-0002-8528-7340",
"clpid": "Thilker-D-A"
},
{
"family_name": "Ubeda",
"given_name": "L.",
"clpid": "Ubeda-L"
},
{
"family_name": "Whitmore",
"given_name": "B. C.",
"clpid": "Whitmore-B-C"
}
],
"abstract": "We use Hubble Space Telescope observations from the Legacy Extragalactic UV Survey to reconstruct the recent star formation histories (SFHs) of three actively star-forming dwarf galaxies, NGC 4449, Holmberg II, and NGC 1705, from their UV color\u2013magnitude diagrams (CMDs). We apply a CMD fitting technique using two independent sets of stellar isochrones, PARSEC-COLIBRI and MIST, to assess the uncertainties related to stellar evolution modeling. Irrespective of the adopted stellar models, all three dwarfs are found to have had almost constant star formation rates (SFRs) in the last 100\u2013200 Myr, with modest enhancements (a factor of ~2) above the 100 Myr averaged SFR. Significant differences among the three dwarfs are found in terms of the overall SFR, the timing of the most recent peak, and the SFR/area. The initial mass function of NGC 1705 and Holmberg II is consistent with a Salpeter slope down to \u22485 M \u2299, whereas it is slightly flatter, s = \u22122.0, in NGC 4449. The SFHs derived with the two different sets of stellar models are consistent with each other, except for some quantitative details, attributable to their input assumptions. They also share the drawback that all synthetic diagrams predict a clear separation in color between the upper main-sequence and helium-burning stars, which is not apparent in the data. Since neither differential reddening, which is significant in NGC 4449, nor unresolved binaries appear to be sufficient to fill the gap, we suggest this calls for a revision of both sets of stellar evolutionary tracks.",
"doi": "10.3847/1538-4357/aab041",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2018-03-20",
"series_number": "1",
"volume": "856",
"issue": "1",
"pages": "Art. No. 62"
},
{
"id": "authors:wc0mt-82g21",
"collection": "authors",
"collection_id": "wc0mt-82g21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180405-154527811",
"type": "article",
"title": "Extinction Maps and Dust-to-gas Ratios in Nearby Galaxies with LEGUS",
"author": [
{
"family_name": "Kahre",
"given_name": "L.",
"orcid": "0000-0002-2037-3096",
"clpid": "Kahre-L"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Van Dyk",
"given_name": "S. D.",
"orcid": "0000-0001-9038-9950",
"clpid": "Van-Dyk-S-D"
}
],
"abstract": "We present a study of the dust-to-gas ratios in five nearby galaxies: NGC 628 (M74), NGC 6503, NGC 7793, UGC 5139 (Holmberg I), and UGC 4305 (Holmberg II). Using Hubble Space Telescopebroadband WFC3/UVIS UV and optical images from the Treasury program Legacy ExtraGalactic UV Survey (LEGUS) combined with archival HST/Advanced Camera for Surveys data, we correct thousands of individual stars for extinction across these five galaxies using an isochrone-matching (reddening-free Q) method. We generate extinction maps for each galaxy from the individual stellar extinctions using both adaptive and fixed resolution techniques and correlate these maps with neutral H I and CO gas maps from the literature, including the H I Nearby Galaxy Survey and the HERA CO-Line Extragalactic Survey. We calculate dust-to-gas ratios and investigate variations in the dust-to-gas ratio with galaxy metallicity. We find a power-law relationship between dust-to-gas ratio and metallicity, consistent with other studies of dust-to-gas ratio compared to metallicity. We find a change in the relation when H2 is not included. This implies that underestimation of N_(H2) in low-metallicity dwarfs from a too-low CO-to-H_2 conversion factor X_(CO) could have produced too low a slope in the derived relationship between dust-to-gas ratio and metallicity. We also compare our extinctions to those derived from fitting the spectral energy distribution (SED) using the Bayesian Extinction and Stellar Tool for NGC 7793 and find systematically lower extinctions from SED fitting as compared to isochrone matching.",
"doi": "10.3847/1538-4357/aab101",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2018-03-10",
"series_number": "2",
"volume": "855",
"issue": "2",
"pages": "Art. No. 133"
},
{
"id": "authors:rw219-tv136",
"collection": "authors",
"collection_id": "rw219-tv136",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180227-103610014",
"type": "article",
"title": "A Study of Two Dwarf Irregular Galaxies with Asymmetrical Star Formation Distributions",
"author": [
{
"family_name": "Hunter",
"given_name": "Deidre A.",
"orcid": "0000-0002-3322-9798",
"clpid": "Hunter-D-A"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Lee",
"given_name": "Janice C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
}
],
"abstract": "Two dwarf irregular galaxies, DDO 187 and NGC 3738, exhibit a striking pattern of star formation: intense star formation is taking place in a large region occupying roughly half of the inner part of the optical galaxy. We use data on the H i distribution and kinematics and stellar images and colors to examine the properties of the environment in the high star formation rate (HSF) halves of the galaxies in comparison with the low star formation rate halves. We find that the pressure and gas density are higher on the HSF sides by 30%\u201370%. In addition we find in both galaxies that the H i velocity fields exhibit significant deviations from ordered rotation and there are large regions of high-velocity dispersion and multiple velocity components in the gas beyond the inner regions of the galaxies. The conditions in the HSF regions are likely the result of large-scale external processes affecting the internal environment of the galaxies and enabling the current star formation there.",
"doi": "10.3847/1538-4357/aaa964",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2018-03-01",
"series_number": "1",
"volume": "855",
"issue": "1",
"pages": "Art. No. 7"
},
{
"id": "authors:gc6g8-pa720",
"collection": "authors",
"collection_id": "gc6g8-pa720",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180405-161427807",
"type": "article",
"title": "The Resolved Stellar Populations in the LEGUS Galaxies1",
"author": [
{
"family_name": "Sabbi",
"given_name": "E.",
"orcid": "0000-0003-2954-7643",
"clpid": "Sabbi-E"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Van Dyk",
"given_name": "S. D.",
"orcid": "0000-0001-9038-9950",
"clpid": "Van-Dyk-S-D"
}
],
"abstract": "The Legacy ExtraGalactic UV Survey (LEGUS) is a multiwavelength Cycle 21 Treasury program on the Hubble Space Telescope. It studied 50 nearby star-forming galaxies in 5 bands from the near-UV to the I-band, combining new Wide Field Camera 3 observations with archival Advanced Camera for Surveys data. LEGUS was designed to investigate how star formation occurs and develops on both small and large scales, and how it relates to the galactic environments. In this paper we present the photometric catalogs for all the apparently single stars identified in the 50 LEGUS galaxies. Photometric catalogs and mosaicked images for all filters are available for download. We present optical and near-UV color\u2013magnitude diagrams for all the galaxies. For each galaxy we derived the distance from the tip of the red giant branch. We then used the NUV color\u2013magnitude diagrams to identify stars more massive than 14 M\u2299, and compared their number with the number of massive stars expected from the GALEX FUV luminosity. Our analysis shows that the fraction of massive stars forming in star clusters and stellar associations is about constant with the star formation rate. This lack of a relation suggests that the timescale for evaporation of unbound structures is comparable or longer than 10 Myr. At low star formation rates this translates to an excess of mass in clustered environments as compared to model predictions of cluster evolution, suggesting that a significant fraction of stars form in unbound systems.",
"doi": "10.3847/1538-4365/aaa8e5",
"issn": "1538-4365",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2018-03",
"series_number": "1",
"volume": "235",
"issue": "1",
"pages": "Art. No. 23"
},
{
"id": "authors:1qdz3-mxf03",
"collection": "authors",
"collection_id": "1qdz3-mxf03",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180202-104540651",
"type": "article",
"title": "iPTF Survey for Cool Transients",
"author": [
{
"family_name": "Adams",
"given_name": "S. M.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Blagorodnova",
"given_name": "N.",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Barlow",
"given_name": "T.",
"clpid": "Barlow-T-A"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Ho",
"given_name": "A. Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "T.",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Neill",
"given_name": "J. D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Walters",
"given_name": "R.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
}
],
"abstract": "We performed a wide-area (2000 deg^2) g and I band experiment as part of a two month extension to the Intermediate Palomar Transient Factory. We discovered 36 extragalactic transients including iPTF17lf, a highly reddened local SN Ia, iPTF17bkj, a new member of the rare class of transitional Ibn/IIn supernovae, and iPTF17be, a candidate luminous blue variable outburst. We do not detect any luminous red novae and place an upper limit on their rate. We show that adding a slow-cadence I band component to upcoming surveys such as the Zwicky Transient Facility will improve the photometric selection of cool and dusty transients.",
"doi": "10.1088/1538-3873/aaa356",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2018-02-01",
"series_number": "985",
"volume": "130",
"issue": "985",
"pages": "Art. No. 034202"
},
{
"id": "authors:qhwvw-n4656",
"collection": "authors",
"collection_id": "qhwvw-n4656",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171211-102818688",
"type": "article",
"title": "The young star cluster population of M51 with LEGUS \u2013 I. A comprehensive study of cluster formation and evolution",
"author": [
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
}
],
"abstract": "Recently acquired WFC3 UV (F275W and F336W) imaging mosaics under the Legacy Extragalactic UV Survey (LEGUS), combined with archival ACS data of M51, are used to study the young star cluster (YSC) population of this interacting system. Our newly extracted source catalogue contains 2834 cluster candidates, morphologically classified to be compact and uniform in colour, for which ages, masses and extinction are derived. In this first work we study the main properties of the YSC population of the whole galaxy, considering a mass-limited sample. Both luminosity and mass functions follow a power-law shape with slope \u22122, but at high luminosities and masses a dearth of sources is observed. The analysis of the mass function suggests that it is best fitted by a Schechter function with slope \u22122 and a truncation mass at 1.00 \u00b1 0.12 \u00d7 10^5 M\u2299. Through Monte Carlo simulations, we confirm this result and link the shape of the luminosity function to the presence of a truncation in the mass function. A mass limited age function analysis, between 10 and 200\u2009Myr, suggests that the cluster population is undergoing only moderate disruption. We observe little variation in the shape of the mass function at masses above 1 \u00d7 10^4 M\u2299\u2009over this age range. The fraction of star formation happening in the form of bound clusters in M51 is \u223c 20\u2009per\u2009cent in the age range 10\u2013100\u2009Myr and little variation is observed over the whole range from 1 to 200\u2009Myr.",
"doi": "10.1093/mnras/stx2403",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2018-01-01",
"series_number": "1",
"volume": "473",
"issue": "1",
"pages": "996-1018"
},
{
"id": "authors:zeqjz-dd973",
"collection": "authors",
"collection_id": "zeqjz-dd973",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170929-091827113",
"type": "article",
"title": "Illuminating Gravitational Waves: A Concordant Picture of Photons from a Neutron Star Merger",
"author": [
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Lau",
"given_name": "R. M.",
"clpid": "Lau-Ryan-M"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Jencson",
"given_name": "J. E.",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-J-E"
},
{
"family_name": "Adams",
"given_name": "S. M.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Blagorodnova",
"given_name": "N.",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "Cannella",
"given_name": "C.",
"orcid": "0000-0003-2667-7290",
"clpid": "Cannella-C-B"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Hallinan",
"given_name": "G.",
"orcid": "0000-0002-7083-4049",
"clpid": "Hallinan-G"
},
{
"family_name": "Harrison",
"given_name": "F.",
"orcid": "0000-0002-4226-8959",
"clpid": "Harrison-F-A"
},
{
"family_name": "Ho",
"given_name": "A. Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Kupfer",
"given_name": "T.",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Madsen",
"given_name": "K.",
"orcid": "0000-0003-1252-4891",
"clpid": "Madsen-K-K"
},
{
"family_name": "Xu",
"given_name": "Y.",
"clpid": "Xu-Yong"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
}
],
"abstract": "Merging neutron stars offer an exquisite laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart (EM170817) to gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic dataset, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma-rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultra-relativistic jets. Instead, we suggest that breakout of a wide-angle, mildly-relativistic cocoon engulfing the jet elegantly explains the low-luminosity gamma-rays, the high-luminosity ultraviolet-optical-infrared and the delayed radio/x-ray emission. We posit that all merging neutron stars may lead to a wide-angle cocoon breakout; sometimes accompanied by a successful jet and sometimes a choked jet.",
"doi": "10.1126/science.aap9455",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "2017-12-22",
"series_number": "6370",
"volume": "358",
"issue": "6370",
"pages": "1559-1565"
},
{
"id": "authors:fhpdv-abe70",
"collection": "authors",
"collection_id": "fhpdv-abe70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171219-083803156",
"type": "article",
"title": "iPTF 16asu: A Luminous, Rapidly Evolving, and High-velocity Supernova",
"author": [
{
"family_name": "Whitesides",
"given_name": "L.",
"clpid": "Whitesides-L"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-R"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Blagorodnova",
"given_name": "N.",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "Cao",
"given_name": "Y.",
"orcid": "0000-0002-8036-8491",
"clpid": "Cao-Yi"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
}
],
"abstract": "Wide-field surveys are discovering a growing number of rare transients whose physical origin is not yet well understood. Here we present optical and UV data and analysis of intermediate Palomar Transient Factory (iPTF) 16asu, a luminous, rapidly evolving, high-velocity, stripped-envelope supernova (SN). With a rest-frame rise time of just four days and a peak absolute magnitude of M_g = -20.4 mag, the light curve of iPTF 16asu is faster and more luminous than that of previous rapid transients. The spectra of iPTF 16asu show a featureless blue continuum near peak that develops into an SN Ic-BL spectrum on the decline. We show that while the late-time light curve could plausibly be powered by ^(56)Ni decay, the early emission requires a different energy source. Nondetections in the X-ray and radio strongly constrain the energy coupled to relativistic ejecta to be at most comparable to the class of low-luminosity gamma-ray bursts (GRBs). We suggest that the early emission may have been powered by either a rapidly spinning-down magnetar or by shock breakout in an extended envelope of a very energetic explosion. In either scenario a central engine is required, making iPTF 16asu an intriguing transition object between superluminous SNe, SNe Ic-BL, and low-luminosity GRBs.",
"doi": "10.3847/1538-4357/aa99de",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-12-20",
"series_number": "2",
"volume": "851",
"issue": "2",
"pages": "Art. No. 107"
},
{
"id": "authors:azsza-5zt29",
"collection": "authors",
"collection_id": "azsza-5zt29",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170713-104625485",
"type": "article",
"title": "Hierarchical Star Formation in Turbulent Media: Evidence from Young Star Clusters",
"author": [
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-K"
},
{
"family_name": "Elmegreen",
"given_name": "B. G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-B-G"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Aloisi",
"given_name": "A.",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-A"
},
{
"family_name": "Bright",
"given_name": "S. N.",
"clpid": "Bright-S-N"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Fumagalli",
"given_name": "M.",
"orcid": "0000-0001-6676-3842",
"clpid": "Fumagalli-M"
},
{
"family_name": "Gallagher",
"given_name": "J. S., III",
"orcid": "0000-0001-8608-0408",
"clpid": "Gallagher-J-S-III"
},
{
"family_name": "Gouliermis",
"given_name": "D. A.",
"orcid": "0000-0002-2763-0075",
"clpid": "Gouliermis-D-A"
},
{
"family_name": "Grebel",
"given_name": "E. K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-E-K"
},
{
"family_name": "Kahre",
"given_name": "L.",
"orcid": "0000-0002-2037-3096",
"clpid": "Kahre-L"
},
{
"family_name": "Kim",
"given_name": "H.",
"clpid": "Kim-H"
},
{
"family_name": "Krumholz",
"given_name": "M. R.",
"orcid": "0000-0003-3893-854X",
"clpid": "Krumholz-M-R"
},
{
"family_name": "Lee",
"given_name": "J. C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Ryon",
"given_name": "J. E.",
"clpid": "Ryon-J-E"
},
{
"family_name": "Ubeda",
"given_name": "L.",
"clpid": "Ubeda-L"
}
],
"abstract": "We present an analysis of the positions and ages of young star clusters in eight local galaxies to investigate the connection between the age difference and separation of cluster pairs. We find that star clusters do not form uniformly but instead are distributed so that the age difference increases with the cluster pair separation to the 0.25\u20130.6 power, and that the maximum size over which star formation is physically correlated ranges from ~200 pc to ~1 kpc. The observed trends between age difference and separation suggest that cluster formation is hierarchical both in space and time: clusters that are close to each other are more similar in age than clusters born further apart. The temporal correlations between stellar aggregates have slopes that are consistent with predictions of turbulence acting as the primary driver of star formation. The velocity associated with the maximum size is proportional to the galaxy's shear, suggesting that the galactic environment influences the maximum size of the star-forming structures.",
"doi": "10.3847/1538-4357/aa740b",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-06-10",
"series_number": "1",
"volume": "842",
"issue": "1",
"pages": "Art. No. 25"
},
{
"id": "authors:s5w8h-f2591",
"collection": "authors",
"collection_id": "s5w8h-f2591",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170623-083724464",
"type": "article",
"title": "Legacy ExtraGalactic UV Survey with The Hubble Space Telescope: Stellar Cluster Catalogs and First Insights Into Cluster Formation and Evolution in NGC 628",
"author": [
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Martin",
"given_name": "C.",
"orcid": "0000-0002-8650-1644",
"clpid": "Martin-D-Christopher"
},
{
"family_name": "Lee",
"given_name": "J. C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
}
],
"abstract": "We report the large effort that is producing comprehensive high-level young star cluster (YSC) catalogs for a significant fraction of galaxies observed with the Legacy ExtraGalactic UV Survey (LEGUS) Hubble treasury program. We present the methodology developed to extract cluster positions, verify their genuine nature, produce multiband photometry (from NUV to NIR), and derive their physical properties via spectral energy distribution fitting analyses. We use the nearby spiral galaxy NGC 628 as a test case for demonstrating the impact that LEGUS will have on our understanding of the formation and evolution of YSCs and compact stellar associations within their host galaxy. Our analysis of the cluster luminosity function from the UV to the NIR finds a steepening at the bright end and at all wavelengths suggesting a dearth of luminous clusters. The cluster mass function of NGC 628 is consistent with a power-law distribution of slopes ~-2 and a truncation of a few times 10^5 M\u2299. After their formation, YSCs and compact associations follow different evolutionary paths. YSCs survive for a longer time frame, confirming their being potentially bound systems. Associations disappear on timescales comparable to hierarchically organized star-forming regions, suggesting that they are expanding systems. We find mass-independent cluster disruption in the inner region of NGC 628, while in the outer part of the galaxy there is little or no disruption. We observe faster disruption rates for low mass (\u226410^4 M\u2299) clusters, suggesting that a mass-dependent component is necessary to fully describe the YSC disruption process in NGC 628.",
"doi": "10.3847/1538-4357/aa7132",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-06-01",
"series_number": "2",
"volume": "841",
"issue": "2",
"pages": "Art. No. 131"
},
{
"id": "authors:08fg7-xnn81",
"collection": "authors",
"collection_id": "08fg7-xnn81",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170531-104615329",
"type": "article",
"title": "Effective Radii of Young, Massive Star Clusters in Two LEGUS Galaxies",
"author": [
{
"family_name": "Ryon",
"given_name": "J. E.",
"clpid": "Ryon-J-E"
},
{
"family_name": "Gallagher",
"given_name": "J. S.",
"clpid": "Gallagher-J-S"
},
{
"family_name": "Smith",
"given_name": "L. J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-L-J"
},
{
"family_name": "Adamo",
"given_name": "A.",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Bright",
"given_name": "S. N.",
"clpid": "Bright-S-N"
},
{
"family_name": "Cignoni",
"given_name": "M.",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-M"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Elmegreen",
"given_name": "B. E.",
"clpid": "Elmegreen-B-E"
},
{
"family_name": "Fumagalli",
"given_name": "M.",
"orcid": "0000-0001-6676-3842",
"clpid": "Fumagalli-M"
},
{
"family_name": "Gouliermis",
"given_name": "D. A.",
"orcid": "0000-0002-2763-0075",
"clpid": "Gouliermis-D-A"
},
{
"family_name": "Grasha",
"given_name": "K.",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-K"
},
{
"family_name": "Grebel",
"given_name": "E. K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-E-K"
},
{
"family_name": "Kim",
"given_name": "H.",
"clpid": "Kim-H"
},
{
"family_name": "Messa",
"given_name": "M.",
"orcid": "0000-0003-1427-2456",
"clpid": "Messa-M"
},
{
"family_name": "Thilker",
"given_name": "D.",
"clpid": "Thilker-D"
},
{
"family_name": "Ubeda",
"given_name": "L.",
"clpid": "Ubeda-L"
}
],
"abstract": "We present a study of the effective (half-light) radii and other structural properties of a systematically selected sample of young, massive star clusters (\u22655 \u00d7 10^3 M\u2299 and \u2264200 Myr) in two nearby spiral galaxies, NGC 628 and NGC 1313. We use Hubble Space Telescope (HST) WFC3/UVIS and archival ACS/WFC data obtained by the Legacy Extragalactic UV Survey (LEGUS), an HST Treasury Program. We measure effective radii with GALFIT, a two-dimensional image-fitting package, and with a new technique to estimate effective radii from the concentration index of observed clusters. The distribution of effective radii from both techniques spans ~0.5\u201310 pc and peaks at 2\u20133 pc for both galaxies. We find slight positive correlations between effective radius and cluster age in both galaxies, but no significant relationship between effective radius and galactocentric distance. Clusters in NGC 1313 display a mild increase in effective radius with cluster mass, but the trend disappears when the sample is divided into age bins. We show that the vast majority of the clusters in both galaxies are much older than their dynamical times, suggesting they are gravitationally bound objects. We find that about half of the clusters in NGC 628 are underfilling their Roche lobes, based on their Jacobi radii. Our results suggest that the young, massive clusters in NGC 628 and NGC 1313 are expanding, due to stellar mass loss or two-body relaxation, and are not significantly influenced by the tidal fields of their host galaxies.",
"doi": "10.3847/1538-4357/aa719e",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-06-01",
"series_number": "2",
"volume": "841",
"issue": "2",
"pages": "Art. No. 92"
},
{
"id": "authors:jbtqq-f3r28",
"collection": "authors",
"collection_id": "jbtqq-f3r28",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170419-090643097",
"type": "article",
"title": "SPIRITS: Uncovering Unusual Infrared Transients with Spitzer",
"author": [
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Masci",
"given_name": "Frank",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-J-E"
},
{
"family_name": "Tinyanont",
"given_name": "Samaporn",
"orcid": "0000-0002-1481-4676",
"clpid": "Tinyanont-S"
},
{
"family_name": "Cao",
"given_name": "Yi",
"orcid": "0000-0002-8036-8491",
"clpid": "Cao-Yi"
},
{
"family_name": "Armus",
"given_name": "Lee",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Lau",
"given_name": "Ryan M.",
"clpid": "Lau-Ryan-M"
},
{
"family_name": "Moore",
"given_name": "Anna",
"orcid": "0000-0002-2894-6936",
"clpid": "Moore-A-M"
},
{
"family_name": "O'Sullivan",
"given_name": "Donal",
"orcid": "0000-0002-4959-9179",
"clpid": "O'Sullivan-Donal"
},
{
"family_name": "Perez",
"given_name": "Andres",
"clpid": "Perez-Andres"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Van Dyk",
"given_name": "Schuyler D.",
"orcid": "0000-0001-9038-9950",
"clpid": "Van-Dyk-S-D"
}
],
"abstract": "We present an ongoing, five-year systematic search for extragalactic infrared transients, dubbed SPIRITS\u2014SPitzer InfraRed Intensive Transients Survey. In the first year, using Spitzer/IRAC, we searched 190 nearby galaxies with cadence baselines of one month and six months. We discovered over 1958 variables and 43 transients. Here, we describe the survey design and highlight 14 unusual infrared transients with no optical counterparts to deep limits, which we refer to as SPRITEs (eSPecially Red Intermediate-luminosity Transient Events). SPRITEs are in the infrared luminosity gap between novae and supernovae, with [4.5] absolute magnitudes between \u221211 and \u221214 (Vega-mag) and [3.6]\u2013[4.5] colors between 0.3 mag and 1.6 mag. The photometric evolution of SPRITEs is diverse, ranging from <0.1 mag yr^(\u22121) to >7 mag yr^(\u22121). SPRITEs occur in star-forming galaxies. We present an in-depth study of one of them, SPIRITS 14ajc in Messier 83, which shows shock-excited molecular hydrogen emission. This shock may have been triggered by the dynamic decay of a non-hierarchical system of massive stars that led to either the formation of a binary or a protostellar merger.",
"doi": "10.3847/1538-4357/aa6978",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-04-20",
"series_number": "2",
"volume": "839",
"issue": "2",
"pages": "Art. No. 88"
},
{
"id": "authors:x8by3-61435",
"collection": "authors",
"collection_id": "x8by3-61435",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170601-134218692",
"type": "article",
"title": "Updated 34-band Photometry for the SINGS/KINGFISH Samples of Nearby Galaxies",
"author": [
{
"family_name": "Dale",
"given_name": "D. A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Roussel",
"given_name": "H.",
"clpid": "Roussel-H"
},
{
"family_name": "Turner",
"given_name": "J. A.",
"orcid": "0000-0003-2261-5746",
"clpid": "Turner-J-A"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Bolatto",
"given_name": "A. D.",
"orcid": "0000-0002-5480-5686",
"clpid": "Bolatto-A-D"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176",
"clpid": "Boquien-M"
},
{
"family_name": "Brown",
"given_name": "M. J. I.",
"orcid": "0000-0002-1207-9137",
"clpid": "Brown-M-J-I"
},
{
"family_name": "Calzetti",
"given_name": "D.",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "De Looze",
"given_name": "I.",
"clpid": "De-Looze-I"
},
{
"family_name": "Galametz",
"given_name": "M.",
"orcid": "0000-0002-0283-8689",
"clpid": "Galametz-M"
},
{
"family_name": "Gordon",
"given_name": "K. D.",
"clpid": "Gordon-K-D"
},
{
"family_name": "Groves",
"given_name": "B. A.",
"orcid": "0000-0002-9768-0246",
"clpid": "Groves-B-A"
},
{
"family_name": "Jarrett",
"given_name": "T. H.",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Herrera-Camus",
"given_name": "R.",
"orcid": "0000-0002-2775-0595",
"clpid": "Herrera-Camus-R"
},
{
"family_name": "Hinz",
"given_name": "J. L.",
"clpid": "Hinz-J-L"
},
{
"family_name": "Hunt",
"given_name": "L. K.",
"orcid": "0000-0001-9162-2371",
"clpid": "Hunt-L-K"
},
{
"family_name": "Kennicutt",
"given_name": "R. C.",
"orcid": "0000-0001-5448-1821",
"clpid": "Kennicutt-R-C"
},
{
"family_name": "Murphy",
"given_name": "E. J.",
"orcid": "0000-0001-7089-7325",
"clpid": "Murphy-E-J"
},
{
"family_name": "Rest",
"given_name": "A.",
"clpid": "Rest-A"
},
{
"family_name": "Sandstrom",
"given_name": "K. M.",
"orcid": "0000-0002-4378-8534",
"clpid": "Sandstrom-K-M"
},
{
"family_name": "Smith",
"given_name": "J.-D. T.",
"orcid": "0000-0003-1545-5078",
"clpid": "Smith-J-D-T"
},
{
"family_name": "Tabatabaei",
"given_name": "F. S.",
"clpid": "Tabatabaei-F-S"
},
{
"family_name": "Wilson",
"given_name": "C. D.",
"orcid": "0000-0001-5817-0991",
"clpid": "Wilson-C-D"
}
],
"abstract": "We present an update to the ultraviolet-to-radio database of global broadband photometry for the 79 nearby galaxies that comprise the union of the KINGFISH (Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel) and SINGS (Spitzer Infrared Nearby Galaxies Survey) samples. The 34-band data set presented here includes contributions from observational work carried out with a variety of facilities including GALEX, SDSS, Pan-STARRS1, NOAO, 2MASS, Wide-Field Infrared Survey Explorer, Spitzer, Herschel, Planck, JCMT, and the VLA. Improvements of note include recalibrations of previously published SINGS BVR _CI_C and KINGFISH far-infrared/submillimeter photometry. Similar to previous results in the literature, an excess of submillimeter emission above model predictions is seen primarily for low-metallicity dwarf or irregular galaxies. This 33-band photometric data set for the combined KINGFISH+SINGS sample serves as an important multiwavelength reference for the variety of galaxies observed at low redshift. A thorough analysis of the observed spectral energy distributions is carried out in a companion paper.",
"doi": "10.3847/1538-4357/aa6032",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-03-01",
"series_number": "1",
"volume": "837",
"issue": "1",
"pages": "Art. No. 90"
},
{
"id": "authors:36jnn-g0x19",
"collection": "authors",
"collection_id": "36jnn-g0x19",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170428-105356377",
"type": "article",
"title": "Hierarchical star formation across the grand-design spiral NGC 1566",
"author": [
{
"family_name": "Gouliermis",
"given_name": "Dimitrios A.",
"orcid": "0000-0002-2763-0075",
"clpid": "Gouliermis-D-A"
},
{
"family_name": "Elmegreen",
"given_name": "Bruce G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-B-G"
},
{
"family_name": "Elmegreen",
"given_name": "Debra M.",
"orcid": "0000-0002-1392-3520",
"clpid": "Elmegreen-D-M"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Cignoni",
"given_name": "Michele",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-M"
},
{
"family_name": "Gallagher",
"given_name": "John S., III",
"orcid": "0000-0001-8608-0408",
"clpid": "Gallagher-J-S-III"
},
{
"family_name": "Kennicutt",
"given_name": "Robert C.",
"orcid": "0000-0001-5448-1821",
"clpid": "Kennicutt-R-C"
},
{
"family_name": "Klessen",
"given_name": "Ralf S.",
"orcid": "0000-0002-0560-3172",
"clpid": "Klessen-R-S"
},
{
"family_name": "Sabbi",
"given_name": "Elena",
"orcid": "0000-0003-2954-7643",
"clpid": "Sabbi-E"
},
{
"family_name": "Thilker",
"given_name": "David",
"clpid": "Thilker-D"
},
{
"family_name": "Ubeda",
"given_name": "Leonardo",
"clpid": "Ubeda-L"
},
{
"family_name": "Aloisi",
"given_name": "Alessandra",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-A"
},
{
"family_name": "Adamo",
"given_name": "Angela",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "Daniel",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Grasha",
"given_name": "Kathryn",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-K"
},
{
"family_name": "Grebel",
"given_name": "Eva K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-E-K"
},
{
"family_name": "Johnson",
"given_name": "Kelsey E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-K-E"
},
{
"family_name": "Sacchi",
"given_name": "Elena",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-E"
},
{
"family_name": "Shabani",
"given_name": "Fayezeh",
"clpid": "Shabani-F"
},
{
"family_name": "Smith",
"given_name": "Linda J.",
"orcid": "0000-0002-0806-168X",
"clpid": "Smith-L-J"
},
{
"family_name": "Wofford",
"given_name": "Aida",
"clpid": "Wofford-A"
}
],
"abstract": "We investigate how star formation is spatially organized in the grand-design spiral NGC 1566 from deep Hubble Space Telescope photometry with the Legacy ExtraGalactic UV Survey. Our contour-based clustering analysis reveals 890 distinct stellar conglomerations at various levels of significance. These star-forming complexes are organized in a hierarchical fashion with the larger congregations consisting of smaller structures, which themselves fragment into even smaller and more compact stellar groupings. Their size distribution, covering a wide range in length-scales, shows a power law as expected from scale-free processes. We explain this shape with a simple 'fragmentation and enrichment' model. The hierarchical morphology of the complexes is confirmed by their mass\u2013size relation that can be represented by a power law with a fractional exponent, analogous to that determined for fractal molecular clouds. The surface stellar density distribution of the complexes shows a lognormal shape similar to that for supersonic non-gravitating turbulent gas. Between 50 and 65 per cent of the recently formed stars, as well as about 90 per cent of the young star clusters, are found inside the stellar complexes, located along the spiral arms. We find an age difference between young stars inside the complexes and those in their direct vicinity in the arms of at least 10 Myr. This time-scale may relate to the minimum time for stellar evaporation, although we cannot exclude the in situ formation of stars. As expected, star formation preferentially occurs in spiral arms. Our findings reveal turbulent-driven hierarchical star formation along the arms of a grand-design galaxy.",
"doi": "10.1093/mnras/stx445",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2017-02-21",
"series_number": "1",
"volume": "468",
"issue": "1",
"pages": "509-530"
},
{
"id": "authors:xxsz6-kc078",
"collection": "authors",
"collection_id": "xxsz6-kc078",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161114-131924115",
"type": "article",
"title": "The connection between galaxy environment and the luminosity function slopes of star-forming regions",
"author": [
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "Daniel A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Lee",
"given_name": "Janice C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Thilker",
"given_name": "David",
"orcid": "0000-0002-8528-7340",
"clpid": "Thilker-D-A"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-D"
},
{
"family_name": "Kennicutt",
"given_name": "Robert C.",
"orcid": "0000-0001-5448-1821",
"clpid": "Kennicutt-R-C"
}
],
"abstract": "We present the first study of GALEX far-ultraviolet (FUV) luminosity functions of individual star-forming regions within a sample of 258 nearby galaxies spanning a large range in total stellar mass and star formation properties. We identify \u223c65 000 star-forming regions (i.e. FUV sources), measure each galaxy's luminosity function, and characterize the relationships between the luminosity function slope (\u03b1) and several global galaxy properties. A final sample of 82 galaxies with reliable luminosity functions are used to define these relationships and represent the largest sample of galaxies with the largest range of galaxy properties used to study the connection between luminosity function properties and galaxy environment. We find that \u03b1 correlates with global star formation properties, where galaxies with higher star formation rates and star formation rate densities (\u03a3_(SFR)) tend to have flatter luminosity function slopes. In addition, we find that neither stochastic sampling of the luminosity function in galaxies with low-number statistics nor the effects of blending due to distance can fully account for these trends. We hypothesize that the flatter slopes in high \u03a3_(SFR) galaxies is due to higher gas densities and higher star formation efficiencies which result in proportionally greater numbers of bright star-forming regions. Finally, we create a composite luminosity function composed of star-forming regions from many galaxies and find a break in the luminosity function at brighter luminosities. However, we find that this break is an artefact of varying detection limits for galaxies at different distances.",
"doi": "10.1093/mnras/stw1694",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2016-11-11",
"series_number": "4",
"volume": "462",
"issue": "4",
"pages": "3766-3799"
},
{
"id": "authors:k0fhv-j9g79",
"collection": "authors",
"collection_id": "k0fhv-j9g79",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210309-132139008",
"type": "article",
"title": "Hierarchical star formation across the ring galaxy NGC\u00a06503",
"author": [
{
"family_name": "Gouliermis",
"given_name": "Dimitrios A.",
"orcid": "0000-0002-2763-0075",
"clpid": "Gouliermis-Dimitrios-A"
},
{
"family_name": "Thilker",
"given_name": "David",
"orcid": "0000-0002-8528-7340",
"clpid": "Thilker-David"
},
{
"family_name": "Elmegreen",
"given_name": "Bruce G.",
"orcid": "0000-0002-1723-6330",
"clpid": "Elmegreen-Bruce-G"
},
{
"family_name": "Elmegreen",
"given_name": "Debra M.",
"orcid": "0000-0002-1392-3520",
"clpid": "Elmegreen-Debra-M"
},
{
"family_name": "Calzetti",
"given_name": "Daniela",
"orcid": "0000-0002-5189-8004",
"clpid": "Calzetti-Daniela"
},
{
"family_name": "Lee",
"given_name": "Janice C.",
"orcid": "0000-0002-2278-9407",
"clpid": "Lee-Janice-C"
},
{
"family_name": "Adamo",
"given_name": "Angela",
"orcid": "0000-0002-8192-8091",
"clpid": "Adamo-Angela"
},
{
"family_name": "Aloisi",
"given_name": "Alessandra",
"orcid": "0000-0003-4137-882X",
"clpid": "Aloisi-Alessandra"
},
{
"family_name": "Cignoni",
"given_name": "Michele",
"orcid": "0000-0001-6291-6813",
"clpid": "Cignoni-Michele"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Dale",
"given_name": "Daniel A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-Daniel-A"
},
{
"family_name": "Gallagher",
"given_name": "John S., III",
"orcid": "0000-0001-8608-0408",
"clpid": "Gallagher-John-S-III"
},
{
"family_name": "Grasha",
"given_name": "Kathryn",
"orcid": "0000-0002-3247-5321",
"clpid": "Grasha-Kathryn"
},
{
"family_name": "Grebel",
"given_name": "Eva K.",
"orcid": "0000-0002-1891-3794",
"clpid": "Grebel-Eva-K"
},
{
"family_name": "Herrero Dav\u00f3",
"given_name": "Artemio",
"orcid": "0000-0001-8768-2179",
"clpid": "Herrero-Dav\u00f3-Artemio"
},
{
"family_name": "Hunter",
"given_name": "Deidre A.",
"orcid": "0000-0002-3322-9798",
"clpid": "Hunter-Deidre-A"
},
{
"family_name": "Johnson",
"given_name": "Kelsey E.",
"orcid": "0000-0001-8348-2671",
"clpid": "Johnson-Kelsey-E"
},
{
"family_name": "Kim",
"given_name": "Hwihyun",
"orcid": "0000-0003-4770-688X",
"clpid": "Kim-Hwihyun"
},
{
"family_name": "Nair",
"given_name": "Preethi",
"orcid": "0000-0001-7069-4026",
"clpid": "Nair-Preethi"
},
{
"family_name": "Nota",
"given_name": "Antonella",
"clpid": "Nota-Antonella"
},
{
"family_name": "Pellerin",
"given_name": "Anne",
"orcid": "0000-0003-1887-1966",
"clpid": "Pellerin-Anne"
},
{
"family_name": "Ryon",
"given_name": "Jenna",
"clpid": "Ryon-Jenna"
},
{
"family_name": "Sabbi",
"given_name": "Elena",
"orcid": "0000-0003-2954-7643",
"clpid": "Sabbi-Elena"
},
{
"family_name": "Sacchi",
"given_name": "Elena",
"orcid": "0000-0001-5618-0109",
"clpid": "Sacchi-Elena"
},
{
"family_name": "Smith",
"given_name": "Linda\u00a0J.",
"clpid": "Smith-Linda-J"
},
{
"family_name": "Tosi",
"given_name": "Monica",
"orcid": "0000-0002-0986-4759",
"clpid": "Tosi-Monica"
},
{
"family_name": "Ubeda",
"given_name": "Leonardo",
"clpid": "Ubeda-Leonardo"
},
{
"family_name": "Whitmore",
"given_name": "Brad",
"orcid": "0000-0002-3784-7032",
"clpid": "Whitmore-Bradley-C"
}
],
"abstract": "We present a detailed clustering analysis of the young stellar population across the star-forming ring galaxy NGC 6503, based on the deep Hubble Space Telescope photometry obtained with the Legacy ExtraGalactic UV Survey. We apply a contour-based map analysis technique and identify in the stellar surface density map 244 distinct star-forming structures at various levels of significance. These stellar complexes are found to be organized in a hierarchical fashion with 95\u2009per\u2009cent being members of three dominant super-structures located along the star-forming ring. The size distribution of the identified structures and the correlation between their radii and numbers of stellar members show power-law behaviours, as expected from scale-free processes. The self-similar distribution of young stars is further quantified from their autocorrelation function, with a fractal dimension of \u223c1.7 for length-scales between \u223c20 pc and 2.5 kpc. The young stellar radial distribution sets the extent of the star-forming ring at radial distances between 1 and 2.5 kpc. About 60\u2009per\u2009cent of the young stars belong to the detected stellar structures, while the remaining stars are distributed among the complexes, still inside the ring of the galaxy. The analysis of the time-dependent clustering of young populations shows a significant change from a more clustered to a more distributed behaviour in a time-scale of \u223c60 Myr. The observed hierarchy in stellar clustering is consistent with star formation being regulated by turbulence across the ring. The rotational velocity difference between the edges of the ring suggests shear as the driving mechanism for this process. Our findings reveal the interesting case of an inner ring forming stars in a hierarchical fashion.",
"doi": "10.1093/mnras/stv1325",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2015-10-01",
"series_number": "4",
"volume": "452",
"issue": "4",
"pages": "3508-3528"
}
]