[
{
"id": "authors:f54ws-sp238",
"collection": "authors",
"collection_id": "f54ws-sp238",
"cite_using_url": "https://authors.library.caltech.edu/records/f54ws-sp238",
"type": "article",
"title": "AT 2024wpp: An Extremely Luminous Fast Ultraviolet Transient Powered by Accretion onto a Black Hole",
"author": [
{
"family_name": "Perley",
"given_name": "Daniel A",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Ho",
"given_name": "Anna Y Q"
},
{
"family_name": "McGrath",
"given_name": "Zo\u00eb"
},
{
"family_name": "Camilo",
"given_name": "Michael"
},
{
"family_name": "Sevilla",
"given_name": "Cassie"
},
{
"family_name": "Chen",
"given_name": "Ping"
},
{
"family_name": "Schroeder",
"given_name": "Genevieve"
},
{
"family_name": "Govreen-Segal",
"given_name": "Taya",
"orcid": "0000-0002-4327-2634"
},
{
"family_name": "Bochenek",
"given_name": "Aleksandra"
},
{
"family_name": "Qin",
"given_name": "Yu-Jing",
"orcid": "0000-0003-3658-6026",
"clpid": "Qin-Yu-Jing"
},
{
"family_name": "Gillanders",
"given_name": "James H",
"orcid": "0000-0002-8094-6108"
},
{
"family_name": "Amend",
"given_name": "Benjamin"
},
{
"family_name": "Anderson",
"given_name": "Joseph P"
},
{
"family_name": "Andreoni",
"given_name": "Igor"
},
{
"family_name": "Aryan",
"given_name": "Amar"
},
{
"family_name": "Bellm",
"given_name": "Eric C"
},
{
"family_name": "Bloom",
"given_name": "Joshua S"
},
{
"family_name": "de Boer",
"given_name": "Thomas"
},
{
"family_name": "Carney",
"given_name": "Jonathan"
},
{
"family_name": "Caiazzo",
"given_name": "Ilaria",
"orcid": "0000-0002-4770-5388"
},
{
"family_name": "Chambers",
"given_name": "Ken C"
},
{
"family_name": "Charalampopoulos",
"given_name": "Panos"
},
{
"family_name": "Chen",
"given_name": "Ting-Wan"
},
{
"family_name": "Chen",
"given_name": "Tracy X",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-X"
},
{
"family_name": "Coughlin",
"given_name": "Eric R",
"orcid": "0000-0003-3765-6401"
},
{
"family_name": "Coughlin",
"given_name": "Michael"
},
{
"family_name": "Dennefeld",
"given_name": "Michel"
},
{
"family_name": "Dimitriadis",
"given_name": "Georgios"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Frostig",
"given_name": "Danielle"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay"
},
{
"family_name": "Galbany",
"given_name": "Llu\u00eds"
},
{
"family_name": "Gangopadhyay",
"given_name": "Anjashay"
},
{
"family_name": "Ghendrih",
"given_name": "Melzie"
},
{
"family_name": "Graham",
"given_name": "Matthew J",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Gromadzki",
"given_name": "Mariusz",
"orcid": "0000-0002-1650-1518"
},
{
"family_name": "Groom",
"given_name": "Steven L",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Guti\u00e9rrez",
"given_name": "Claudia P"
},
{
"family_name": "Hinds",
"given_name": "K-Ryan",
"clpid": "Hinds-K-Ryan"
},
{
"family_name": "Huber",
"given_name": "Mark E"
},
{
"family_name": "Inserra",
"given_name": "Cosimo",
"orcid": "0000-0002-3968-4409"
},
{
"family_name": "Kaiser",
"given_name": "Benjamin C"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Koivisto",
"given_name": "Niilo E"
},
{
"family_name": "Lin",
"given_name": "Chien-Cheng",
"orcid": "0000-0002-7272-5129"
},
{
"family_name": "Liu",
"given_name": "Chang",
"orcid": "0000-0002-7866-4531"
},
{
"family_name": "Lowe",
"given_name": "Thomas B"
},
{
"family_name": "Magnier",
"given_name": "Eugene"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Milligan",
"given_name": "Andrew",
"orcid": "0009-0006-6426-2431"
},
{
"family_name": "Minguez",
"given_name": "Paloma"
},
{
"family_name": "Mo",
"given_name": "Geoffrey",
"orcid": "0000-0001-6331-112X",
"clpid": "Mo-Geoffrey"
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "Tom\u00e1s E"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Pessi",
"given_name": "Priscila J",
"orcid": "0000-0002-8041-8559"
},
{
"family_name": "Pignata",
"given_name": "Giuliano"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Rehemtulla",
"given_name": "Nabeel",
"orcid": "0000-0002-5683-2389"
},
{
"family_name": "Rich",
"given_name": "R Michael",
"orcid": "0000-0003-0427-8387"
},
{
"family_name": "Sahu",
"given_name": "Anwesha"
},
{
"family_name": "Singh",
"given_name": "Avinash"
},
{
"family_name": "Smartt",
"given_name": "Stephen J",
"orcid": "0000-0002-8229-1731"
},
{
"family_name": "Smith",
"given_name": "Ian A",
"orcid": "0000-0001-8605-5608"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Srinivasaragavan",
"given_name": "Gokul",
"orcid": "0000-0002-6428-2700",
"clpid": "Srinivasaragavan-Gokul"
},
{
"family_name": "Srivastav",
"given_name": "Shubham"
},
{
"family_name": "Stein",
"given_name": "Robert D",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert-D"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Tweddle",
"given_name": "Jack W"
},
{
"family_name": "Wainscoat",
"given_name": "Richard"
},
{
"family_name": "Wise",
"given_name": "Jacob L"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Young",
"given_name": "David R"
}
],
"abstract": "We present the discovery of AT 2024wpp ('Whippet'), a fast and luminous 18cow-like transient. At a redshift of z = 0.0868, revealed by Keck Cosmic Web Imager spectroscopy of its faint star-forming host, it is the fourth-nearest example of its class to date. Rapid identification of the source in the Zwicky Transient Facility data stream permitted ultraviolet-through-optical observations to be obtained prior to peak, allowing the first determination of the peak bolometric luminosity (2 × 10\u2074\u2075 erg s\u207b¹), maximum photospheric radius (10¹\u2075 cm), and total radiated energy (10\u2075¹ erg) of an 18cow-like object. We present results from a comprehensive multiwavelength observing campaign, including a far-UV spectrum from the Cosmic Origins Spectrograph on the Hubble Space Telescope and deep imaging extending >100 days post-explosion from the Very Large Telescope, Hubble Space Telescope, Very Large Array, and Atacama Large Millimetre Array. We interpret the observations under a model in which a rapidly-accreting central engine blows a fast (∼ 0.2 c) wind into the surrounding medium and irradiates it with X-rays. The high Doppler velocities and intense ionization within this wind prevent identifiable spectroscopic features from appearing in the ejecta or in the surrounding circumstellar material. Weak H and He signatures do emerge in the spectra after 35 days in the form of double-peaked narrow lines. Each peak is individually narrow (full width δv ∼ 3000 km s\u207b¹) but the two components are separated by Δv ∼ 6600 km s\u207b¹, indicating stable structures of denser material, possibly representing streams of tidal ejecta or an ablated companion star.
",
"doi": "10.1093/mnras/stag678",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2026-06",
"series_number": "1",
"volume": "549",
"issue": "1",
"pages": "stag678"
},
{
"id": "authors:t0vsc-k4s10",
"collection": "authors",
"collection_id": "t0vsc-k4s10",
"cite_using_url": "https://authors.library.caltech.edu/records/t0vsc-k4s10",
"type": "article",
"title": "An extremely luminous flare recorded from a supermassive black hole",
"author": [
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "McKernan",
"given_name": "Barry"
},
{
"family_name": "Ford",
"given_name": "K. E. Saavik",
"orcid": "0000-0002-5956-851X"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Cantiello",
"given_name": "Matteo"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Ding",
"given_name": "Yuanze",
"orcid": "0000-0002-5770-2666",
"clpid": "Ding-Yuanze"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Koss",
"given_name": "Mike",
"orcid": "0000-0002-7998-9581"
},
{
"family_name": "Margutti",
"given_name": "Raffaella",
"orcid": "0000-0003-4768-7586"
},
{
"family_name": "Rose",
"given_name": "Sam",
"orcid": "0000-0003-4725-4481",
"clpid": "Rose-Sam"
},
{
"family_name": "Somalwar",
"given_name": "Jean",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Wiseman",
"given_name": "Phil"
},
{
"family_name": "Djorgovski",
"given_name": "S. G.",
"orcid": "0000-0002-0603-3087",
"clpid": "Djorgovski-S-G"
},
{
"family_name": "Veres",
"given_name": "Patrik M.",
"orcid": "0000-0002-9553-2987"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Chen",
"given_name": "Tracy X.",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-X"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
}
],
"abstract": "\n
\n
Since their discovery more than 60 years ago, accreting supermassive black holes in active galactic nuclei (AGN) have been recognized as highly variable sources, requiring an extremely compact, dynamic environment. Their variability is related to several phenomena, including changing accretion rates, temperature changes, foreground absorbers and structural changes to the accretion disk. Spurred by a new generation of time-domain surveys, the extremes of black hole variability are now being probed. Here we describe the discovery of an extreme flare by the AGN J224554.84+374326.5, which brightened by more than a factor of 40 in 2018. The source has slowly faded since then. The total emitted ultraviolet and optical energy to date is ~1054 erg, which represents the complete conversion of approximately one solar mass into electromagnetic radiation. This flare is 30 times more powerful than the previous most powerful AGN transient. Very few physical events in the Universe can liberate this much electromagnetic energy. We discuss potential mechanisms, including the tidal disruption of a high-mass star (>30 M\u2299), gravitational lensing of an AGN flare or supernova, or a supermassive (pair-instability) supernova in the accretion disk of an AGN. We favour the tidal disruption of a massive star in a prograde orbit in an AGN disk.
\n
\n
The relation between Type Ia supernovae (SNe Ia) and the stellar masses of their host galaxy is well documented. In particular, Hubble residuals display a distinct luminosity shift based on host mass. This is known as the mass step. This effect is widely used as an additional correction factor in the standardisation of SN Ia luminosities. We investigate the Hubble residuals and the mass step of normal SNe Ia in the context of Si\u202fIIλ6355 velocities based on 277 normal SNe Ia that are near their peak in the second data release (DR2) of the Zwicky Transient Facility (ZTF). We divided the sample into high-velocity (HV) and normal-velocity (NV) SNe Ia, separated at 12,000 km s−1. This produced a sample of 70 HV and 207 NV objects. We then explored potential environment- and/or progenitor-related effects by investigating the Si\u202fIIλ6355 velocities with parameters such as the light-curve stretch x1, the colour c, and the host galaxy properties. Although we only find a marginal difference between the Hubble residuals of HV and NV SNe Ia, the NV mass step is 0.149\u2005±\u20050.024 mag (6.3σ). The HV mass step is smaller, 0.046\u2005±\u20050.041 mag (1.1σ), and is consistent with zero. The difference between the NV and HV mass steps is modest, at ∼2.2σ. Moreover, the clearest subtype difference appears for SNe in central regions (dDLR\u2004<\u20041), where NV SNe Ia show a large mass step, whereas HV SNe Ia are consistent with no step, yielding a difference of 3.1–3.6σ between NV and HV SNe Ia. We observe a host-colour step for both subtypes. NV SNe Ia show a step of 0.142\u2005±\u20050.024 mag (5.9σ), while HV SNe Ia show a step of 0.158\u2005±\u20050.042 mag (3.8σ), where the HV SNe Ia step appears to be larger, but the significance is lower because the sample size is smaller. Overall, the NV and HV colour steps are statistically consistent. HV SNe Ia also show modest (∼2.5–3σ) steps in certain subsets, such as those in outer regions (dDLR\u2004>\u20041), whereas NV SNe display stronger environmental trends. Our results indicate that NV SNe Ia appear to be more environmentally sensitive, particularly in central likely metal-rich and older regions, while HV SNe Ia show weaker and subset-dependent trends. This suggests that applying a universal mass-step correction might introduce biases, and that incorporating refined classifications and/or environment-dependent factors, such as the location within the host, might improve future cosmological analyses beyond the standard x1 and c cuts.
",
"doi": "10.1051/0004-6361/202556376",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2026-01",
"volume": "705",
"pages": "A76"
},
{
"id": "authors:xcn46-6f355",
"collection": "authors",
"collection_id": "xcn46-6f355",
"cite_using_url": "https://authors.library.caltech.edu/records/xcn46-6f355",
"type": "article",
"title": "Discovery of SN 2025wny: A Strongly Gravitationally Lensed Superluminous Supernova at z = 2.01",
"author": [
{
"family_name": "Johansson",
"given_name": "Joel",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Wise",
"given_name": "Jacob L.",
"orcid": "0000-0003-0733-2916"
},
{
"family_name": "Qin",
"given_name": "Yu-Jing",
"orcid": "0000-0003-3658-6026",
"clpid": "Qin-Yu-Jing"
},
{
"family_name": "McGrath",
"given_name": "Zo\u00eb",
"orcid": "0009-0006-0726-1328"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Lemon",
"given_name": "Cameron",
"orcid": "0000-0003-2456-9317"
},
{
"family_name": "Gangopadhyay",
"given_name": "Anjasha",
"orcid": "0000-0002-3884-5637"
},
{
"family_name": "Tsalapatas",
"given_name": "Konstantinos",
"orcid": "0009-0004-1062-8886"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Fransson",
"given_name": "Claes",
"orcid": "0000-0001-8532-3594"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Gruen",
"given_name": "Daniel",
"orcid": "0000-0003-3270-7644"
},
{
"family_name": "Hall",
"given_name": "Xander J.",
"orcid": "0000-0002-9364-5419"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi",
"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": "Lunnan",
"given_name": "Ragnhild",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "M\u00f6rtsell",
"given_name": "Edvard",
"orcid": "0000-0002-8380-6143"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Hjortlund",
"given_name": "Jacob Osman",
"orcid": "0009-0009-6243-8300"
},
{
"family_name": "Rich",
"given_name": "R. Michael",
"orcid": "0000-0003-0427-8387"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Singh",
"given_name": "Avinash",
"orcid": "0000-0003-2091-622X"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Townsend",
"given_name": "Alice",
"orcid": "0000-0001-6343-3362"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We present the discovery of SN 2025wny (ZTF25abnjznp/GOTO25gqt) and spectroscopic classification of this event as the first gravitationally lensed Type I superluminous supernova (SLSN-I). Deep ground-based follow-up observations resolve four images of the supernova with ∼1.″7 angular separation from the main lens galaxy, each coincident with the lensed images of a background galaxy seen in archival imaging of the field. Spectroscopy of the brightest image shows narrow features matching absorption lines at a redshift of z = 2.010 and broad features matching those seen in superluminous SNe with far-UV coverage. We infer a magnification factor of μ ∼ 20–50 for the brightest image in the system, based on photometric and spectroscopic comparisons to other SLSNe-I. SN 2025wny demonstrates that gravitationally lensed SNe are in reach of ground-based facilities out to redshifts far higher than previously assumed, and provide a unique window into studying distant supernovae and the internal properties of dwarf galaxies, as well as for time-delay cosmography.
",
"doi": "10.3847/2041-8213/ae1d61",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-12-10",
"series_number": "1",
"volume": "995",
"issue": "1",
"pages": "L17"
},
{
"id": "authors:r494d-8jk37",
"collection": "authors",
"collection_id": "r494d-8jk37",
"cite_using_url": "https://authors.library.caltech.edu/records/r494d-8jk37",
"type": "article",
"title": "Prediscovery Activity of New Interstellar Object 3I/ATLAS: Rapid Brightening from 6 to 4 au",
"author": [
{
"family_name": "Ye \u53f6",
"given_name": "Quanzhi \u6cc9\u5fd7",
"orcid": "0000-0002-4838-7676"
},
{
"family_name": "Kelley",
"given_name": "Michael S. P.",
"orcid": "0000-0002-6702-7676"
},
{
"family_name": "Hsieh",
"given_name": "Henry H.",
"orcid": "0000-0001-7225-9271"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"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": "Drake",
"given_name": "Andrew",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
}
],
"abstract": "We report on the prediscovery observations and constraints of the new interstellar comet 3I/2025 N1 (ATLAS), made by the Zwicky Transient Facility, for the inbound leg of the comet out to a heliocentric distance of rh = 17 au, or approximately a year before its discovery. We find that 3I/ATLAS has been active inward of a heliocentric distance of at least rh = 6.5 au. The comet followed a brightening rate of ∝ r_h^(−3.8), which is significantly steeper than that of the only other known interstellar comet, 2I/Borisov, and is more consistent with dynamically old long-period comets and short-period comets in the solar system. By measuring the brightening of the dust coma, we estimate that 3I had a dust production rate of M_d \u0307 ∼ 5 kg s\u207b¹ in 2025 early May (rh ∼ 6 au), increasing to M_d \u0307 ∼ 5 kg s\u207b¹ toward 2025 mid-July (rh ∼ 4 au) assuming 100 μm dust grains, in line with the more recent Hubble Space Telescope measurement made at rh = 3.8 au. Comparison with the prediscovery photometry by the Transiting Exoplanet Survey Satellite suggested that 3I started producing constant dust outflow probably around rh ∼ 9 au, coinciding with the turn-on distance of CO2 ice. We also conduct a deep search of 3I/ATLAS with multiple nights of data taken in 2024, when the comet was at rh = 13–17 au, and conclude that the comet was no brighter than 2–5 mag above the coma or bare-nucleus lightcurves. This suggests that the comet did not exhibit strong outbursts during these periods, consistent with 2I/Borisov as well as most long-period solar system comets.
",
"doi": "10.3847/2041-8213/ae147b",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-11-01",
"series_number": "1",
"volume": "993",
"issue": "1",
"pages": "L31"
},
{
"id": "authors:27mz4-j6510",
"collection": "authors",
"collection_id": "27mz4-j6510",
"cite_using_url": "https://authors.library.caltech.edu/records/27mz4-j6510",
"type": "article",
"title": "ZTF SN Ia DR2: Cosmology-independent constraints on Type Ia supernova standardisation from supernova siblings",
"author": [
{
"family_name": "Dhawan",
"given_name": "S.",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Mortsell",
"given_name": "E.",
"orcid": "0000-0002-8380-6143"
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Smith",
"given_name": "M."
},
{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Dimitriadis",
"given_name": "G.",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Nugent",
"given_name": "P. E.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Galbany",
"given_name": "L.",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Kenworthy",
"given_name": "W. D.",
"orcid": "0000-0002-5153-5983"
},
{
"family_name": "de Jaeger",
"given_name": "T.",
"orcid": "0000-0001-6069-1139"
},
{
"family_name": "Terwel",
"given_name": "J. H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Kim",
"given_name": "Y.-L.",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Burgaz",
"given_name": "U.",
"orcid": "0000-0003-0126-3999"
},
{
"family_name": "Rosnet",
"given_name": "P.",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Purdum",
"given_name": "J.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Laher",
"given_name": "R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Healy",
"given_name": "B.",
"clpid": "Healy-B"
}
],
"abstract": "Understanding Type Ia supernovae (SNe Ia) and the empirical standardisation relations that make them excellent distance indicators is vital to improving cosmological constraints. SN Ia ‘siblings, i.e. two or more SNe Ia in the same host or parent galaxy, offer a unique way to infer the standardisation relations and their scatter across the population. We analysed a sample of 25 SN Ia pairs observed homogeneously by the Zwicky Transient Facility (ZTF) to infer the SNe Ia light curve width-luminosity and colour-luminosity parameters, α and β. Using the pairwise constraints from siblings, which allow for a scatter in the standardisation relations, we found α\u2004=\u20040.218\u2005±\u20050.055 and β\u2004=\u20043.084\u2005±\u20050.312, respectively, with a dispersion in α and β of ≤0.195 and ≤0.923, respectively, at a 95% confidence level. While the median dispersion is large, the values within ∼1σ are consistent with no dispersion. Hence, fitting for a single global standardisation relation, we found α\u2004=\u20040.228\u2005±\u20050.029 and β\u2004=\u20043.160\u2005±\u20050.191. We also found a very small intrinsic scatter of the siblings sample σint\u2004≤\u20040.10 mag at a 95% confidence level compared to σint\u2004=\u20040.22\u2005±\u20050.04 mag when computing the scatter using the Hubble residuals without comparing them as siblings. When comparing to large samples used in cosmological measurements, we found an α that is ∼2-3 σ higher, while the β values are consistent. The high α is driven by low x1 pairs, potentially suggesting that the slow and fast declining SN Ia have different slopes for the width-luminosity relation. We found no difference in α and β when dividing the sample by host galaxy mass. The finding of a higher α with increased statistics can be confirmed or refuted through upcoming time-domain surveys. If confirmed, this finding can improve the cosmological inference from SNe Ia and be used to infer properties of the progenitors for subpopulations of SNe Ia.
",
"doi": "10.1051/0004-6361/202450392",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2025-10",
"volume": "702",
"pages": "A190"
},
{
"id": "authors:hjgt4-w2z11",
"collection": "authors",
"collection_id": "hjgt4-w2z11",
"cite_using_url": "https://authors.library.caltech.edu/records/hjgt4-w2z11",
"type": "article",
"title": "A ZTF Search for Circumstellar Debris Transits in White Dwarfs: Six New Candidates, One with Gas Disk Emission, Identified in a Novel Metric Space",
"author": [
{
"family_name": "Bhattacharjee",
"given_name": "Soumyadeep",
"orcid": "0000-0003-2071-2956",
"clpid": "Bhattacharjee-Soumyadeep"
},
{
"family_name": "Vanderbosch",
"given_name": "Zachary P.",
"orcid": "0000-0002-0853-3464",
"clpid": "Vanderbosch-Zachary-P"
},
{
"family_name": "Hollands",
"given_name": "Mark A.",
"orcid": "0000-0003-0089-2080"
},
{
"family_name": "Tremblay",
"given_name": "Pier-Emmanuel",
"orcid": "0000-0001-9873-0121"
},
{
"family_name": "Xu \u8bb8",
"given_name": "Siyi \u5072\u827a",
"orcid": "0000-0002-8808-4282"
},
{
"family_name": "Guidry",
"given_name": "Joseph A.",
"orcid": "0000-0001-9632-7347"
},
{
"family_name": "Hermes",
"given_name": "J. J.",
"orcid": "0000-0001-5941-2286"
},
{
"family_name": "Caiazzo",
"given_name": "Ilaria",
"orcid": "0000-0002-4770-5388"
},
{
"family_name": "Rodriguez",
"given_name": "Antonio C.",
"orcid": "0000-0003-4189-9668",
"clpid": "Rodriguez-Antonio-C"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872"
},
{
"family_name": "El-Badry",
"given_name": "Kareem",
"orcid": "0000-0002-6871-1752",
"clpid": "El-Badry-Kareem"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Roulston",
"given_name": "Benjamin R.",
"orcid": "0000-0002-9453-7735"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Toloza",
"given_name": "Odette",
"orcid": "0000-0002-2398-719X"
}
],
"abstract": "\n
White dwarfs (WDs) showing transits from orbiting planetary debris provide significant insights into the structure and dynamics of debris disks, which are eventually accreted to produce metal pollution. This is a rare class of objects with only eight published systems. In this work, we perform a systematic search for such systems within 500 pc in the Gaia-eDR3 catalog of WDs using the light curves from the Zwicky Transient Facility (ZTF) and present six new candidates. Our selection process targets the top 1% most photometrically variable sources identified using a combined variability metric from ZTF and Gaia eDR3 photometry, boosted by a metric space we define using von Neumann statistics and Pearson-Skew as a novel discovery tool to identify these systems. This is followed by optical spectroscopic observations of visually selected variables to confirm metal pollution. Four of the six systems show long-timescale photometric variability spanning several months to years, resulting either from long-term evolution of transit activity or dust and debris clouds at wide orbits. Among them, WD J1013–0427 shows an indication of reddening during the long-duration dip. Interpreting this as dust extinction makes it the first system to indicate an abundance of dust grains with radius \u22720.3 μm in the occulting material. The same object also shows metal emission lines that map an optically thick eccentric gas disk orbiting within the star’s Roche limit. For each candidate, we infer the abundances of the photospheric metals and estimate accretion rates. We show that transiting debris systems tend to have higher inferred accretion rates compared to the general population of metal-polluted WDs. Growing the number of these systems will further illuminate such comparative properties in the near future. Separately, we also serendipitously discovered an AM Canis Venaticorum showing a very long-duration outburst—only the fourth such system to be known.
\n
Tidal disruption events (TDEs) that are spatially offset from the nuclei of their host galaxies offer a new probe of massive black hole (MBH) wanderers, binaries, triples, and recoiling MBHs. Here we present AT2024tvd, the first off-nuclear TDE identified through optical sky surveys. High-resolution imaging with the Hubble Space Telescope shows that AT2024tvd is 0914 ± 0010 offset from the apparent center of its host galaxy, corresponding to a projected distance of 0.808 ± 0.009 kpc at z = 0.045. Chandra and Very Large Array observations support the same conclusion for the TDE's X-ray and radio emission. AT2024tvd exhibits typical properties of nuclear TDEs, including a persistent hot UV/optical component that peaks at Lbb ∼ 6 × 1043 erg s−1, broad hydrogen lines in its optical spectra, and delayed brightening of luminous (LX,peak ∼ 3 × 1043 erg s−1), highly variable soft X-ray emission. The MBH mass of AT2024tvd is 106±1 M\u2299, at least 10 times lower than its host galaxy's central black hole mass (\u2273108 M\u2299). The MBH in AT2024tvd has two possible origins: a wandering MBH from the lower-mass galaxy in a minor merger during the dynamical friction phase or a recoiling MBH ejected by triple interactions. Combining AT2024tvd with two previously known off-nuclear TDEs discovered in X-rays (3XMM J2150 and EP240222a), which likely involve intermediate-mass black holes in satellite galaxies, we find that the parent galaxies of all three events are very massive (∼1010.9 M\u2299). This result aligns with expectations from cosmological simulations that the number of offset MBHs scales linearly with the host halo mass.
",
"doi": "10.3847/2041-8213/add7de",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-06-01",
"series_number": "2",
"volume": "985",
"issue": "2",
"pages": "L48"
},
{
"id": "authors:zc70w-ew217",
"collection": "authors",
"collection_id": "zc70w-ew217",
"cite_using_url": "https://authors.library.caltech.edu/records/zc70w-ew217",
"type": "article",
"title": "The First Systematically Identified Repeating Partial Tidal Disruption Event",
"author": [
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Ravi",
"given_name": "Vikram",
"orcid": "0000-0002-7252-5485",
"clpid": "Ravi-Vikram"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509"
},
{
"family_name": "Guolo",
"given_name": "Muryel",
"orcid": "0000-0002-5063-0751"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Lu",
"given_name": "Wenbin",
"orcid": "0000-0002-1568-7461"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
}
],
"abstract": "\n
Tidal disruption events (TDEs) occur when a star enters the tidal radius of a supermassive black hole. If the star only grazes the tidal radius, a fraction of the stellar mass will be accreted in a partial TDE (pTDE). The remainder can continue orbiting and may be redisrupted at pericenter, causing a repeating pTDE. pTDEs may be as or more common than full TDEs, yet few are known. In this work, we present the discovery of the first repeating pTDE from a systematically selected sample, AT 2020vdq. AT 2020vdq was originally identified as an optically and radio-flaring TDE. Around 947 days after its discovery, it rebrightened dramatically in the optical. The optical flare was remarkably fast and luminous given its black hole mass compared to previous TDEs. It was accompanied by extremely broad (∼0.1c) optical/UV spectral features and faint X-ray emission (LX ∼ 3 × 1041 erg s−1), but no new radio-emitting component. Based on the transient optical/UV spectral features and the broadband lightcurve, we show that AT 2020vdq is a repeating pTDE. We then use it to constrain TDE models; in particular, we favor a star originally in a very tight binary system that is tidally broken apart by the Hills mechanism. We also constrain the repeating pTDE rate to be 10−6–10−5 yr−1 galaxy−1, with uncertainties dominated by the unknown distribution of pTDE repeat timescales. In the Hills framework, this means the binary fraction in the galactic nucleus is of the order of a few percent.
\n
We present observations of the Type IIP supernova (SN) SN 2024jlf, including spectroscopy beginning just 0.7 days (∼17 hr) after first light. Rapid follow-up was enabled by the new BTSbot-nearby program, which involves autonomously triggering target-of-opportunity requests for new transients in Zwicky Transient Facility data that are coincident with nearby (D < 60 Mpc) galaxies and identified by the BTSbot machine learning model. Early photometry and nondetections shortly prior to first light show that SN 2024jlf initially brightened by >4 mag day−1, quicker than ∼90% of Type II SNe. Early spectra reveal weak flash ionization features: narrow, short-lived (1.3 < τ[days] < 1.8) emission lines of Hα, He ii, and C iv. Assuming a wind velocity of vw = 50 km s−1, these properties indicate that the red supergiant progenitor exhibited enhanced mass loss in the last year before explosion. We constrain the mass-loss rate to 10\u207b\u2074 < M [M\u2299 yr\u207b¹] < 10\u207b³ by matching observations to model grids from two independent radiative hydrodynamics codes. BTSbot-nearby automation minimizes spectroscopic follow-up latency, enabling the observation of ephemeral early-time phenomena exhibited by transients.
",
"doi": "10.3847/1538-4357/adcf1e",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2025-06-01",
"series_number": "2",
"volume": "985",
"issue": "2",
"pages": "241"
},
{
"id": "authors:1fx63-j9d02",
"collection": "authors",
"collection_id": "1fx63-j9d02",
"cite_using_url": "https://authors.library.caltech.edu/records/1fx63-j9d02",
"type": "article",
"title": "VLASS Tidal Disruption Events with Optical Flares. I. The Sample and a Comparison to Optically Selected TDEs",
"author": [
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Ravi",
"given_name": "Vikram",
"orcid": "0000-0002-7252-5485",
"clpid": "Ravi-Vikram"
},
{
"family_name": "Dong",
"given_name": "Dillon Z.",
"orcid": "0000-0001-9584-2531",
"clpid": "Dong-Dillon-Z"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Hallinan",
"given_name": "Gregg",
"orcid": "0000-0002-7083-4049",
"clpid": "Hallinan-G"
},
{
"family_name": "Law",
"given_name": "Casey",
"orcid": "0000-0002-4119-9963",
"clpid": "Law-Casey"
},
{
"family_name": "Miller",
"given_name": "Jessie",
"orcid": "0000-0001-8840-922X",
"clpid": "Miller-Jessie"
},
{
"family_name": "Myers",
"given_name": "Steven T."
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
}
],
"abstract": "\n
In this work, we use the Jansky Very Large Array Sky Survey to compile the first sample of six radio-selected tidal disruption events (TDEs) with transient optical counterparts. While we still lack the statistics to do detailed population studies of radio-selected TDEs, we use these events to suggest trends in host galaxy and optical light-curve properties that may correlate with the presence of radio emission and hence can inform optically selected TDE radio follow-up campaigns. We find tentative trends that radio-selected TDEs tend to have faint and cool optical flares, as well as host galaxies with low supermassive black hole masses, although larger samples are required to establish these trends as statistically significant. Our radio-selected TDEs also tend to have more energetic, larger radio-emitting regions than radio-detected, optically selected TDEs. We consider possible explanations for these trends, including by invoking super-Eddington accretion and enhanced circumnuclear media. Finally, we constrain the radio-emitting TDE rate to be \u227310 Gpc−3 yr−1.
\n
Context. As type Ia supernova cosmology transitions from a statistics-dominated to a systematics-dominated era, it is crucial to understand the remaining unexplained uncertainties that affect their luminosity, such as those stemming from astrophysical biases. Type Ia supernovae are standardisable candles whose absolute magnitude reaches a scatter of typically 0.15 mag when empirical correlations with their light-curve stretch and colour and with their environmental properties are accounted for.
\nAims. We investigate the dependence of the standardisation process of type Ia supernovae on the astrophysical environment to ultimately reduce their scatter in magnitude. We focus on colour standardisation.
\nMethods. We used the volume-limited ZTF SN Ia DR2 sample, which offers unprecedented statistics for the low-redshift (z\u2004<\u20040.06) range. We first studied the colour distribution with a focus on the effects of dust to then select a dustless subsample of objects that originated in environments with a low stellar mass and in the outskirts of their host galaxies. We then examined the colour-residual relation and its associated parameter β. Finally, we investigated the colour dependence of the environment-dependent magnitude offsets (steps) to separate their intrinsic and extrinsic components.
\nResults. Our sample of nearly 1000 supernovae probes the red tail of the colour distribution up to c\u2004=\u20040.8. The dustless sample exhibits a significantly shorter red tail (4.3σ) than the whole sample, but the distributions around c\u2004∼\u20040 are similar for both samples. This suggests that the reddening above c\u2004≥\u20040.2 is dominated by interstellar dust absorption of the host and that the remaining colour scatter has an intrinsic origin. The colour-residual relation is linear with light-curve colour. We found indications of a potential evolution of β with the stellar host mass, with β\u2004∼\u20043.6 for low-mass galaxies, compared to β\u2004=\u20043.05\u2005±\u20050.06 for the full sample. Finally, in contrast to recent claims from the literature, we found no evolution of steps as a function of light-curve colour. This suggests that dust may not be the dominating mechanism for the dependence on the environment of the magnitude of type Ia supernovae.
",
"doi": "10.1051/0004-6361/202450943",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A4"
},
{
"id": "authors:ck40a-pj869",
"collection": "authors",
"collection_id": "ck40a-pj869",
"cite_using_url": "https://authors.library.caltech.edu/records/ck40a-pj869",
"type": "article",
"title": "Candidate strongly lensed type Ia supernovae in the Zwicky Transient Facility archive",
"author": [
{
"family_name": "Townsend",
"given_name": "A.",
"orcid": "0000-0001-6343-3362"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Sagu\u00e9s Carracedo",
"given_name": "A.",
"orcid": "0000-0002-3498-2167"
},
{
"family_name": "Kowalski",
"given_name": "M.",
"orcid": "0000-0001-8594-8666"
},
{
"family_name": "Arendse",
"given_name": "N.",
"orcid": "0000-0001-5409-6480"
},
{
"family_name": "Dhawan",
"given_name": "S.",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "M\u00f6rtsell",
"given_name": "E.",
"orcid": "0000-0002-8380-6143"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Fern\u00e1ndez",
"given_name": "E."
},
{
"family_name": "Kim",
"given_name": "A. G.",
"orcid": "0000-0001-6315-8743"
},
{
"family_name": "Nugent",
"given_name": "P. E.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Prada",
"given_name": "F.",
"orcid": "0000-0001-7145-8674"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Sarin",
"given_name": "N.",
"orcid": "0000-0003-2700-1030"
},
{
"family_name": "Sharma",
"given_name": "D."
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Coughlin",
"given_name": "M. W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Dekany",
"given_name": "R.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Lacroix",
"given_name": "L.",
"orcid": "0000-0003-0629-5746"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Aguilar",
"given_name": "J.",
"orcid": "0000-0003-0822-452X"
},
{
"family_name": "Ahlen",
"given_name": "S.",
"orcid": "0000-0001-6098-7247"
},
{
"family_name": "Bailey",
"given_name": "S.",
"orcid": "0000-0003-4162-6619"
},
{
"family_name": "Brooks",
"given_name": "D."
},
{
"family_name": "Claybaugh",
"given_name": "T.",
"orcid": "0000-0002-5024-6987"
},
{
"family_name": "de la Macorra",
"given_name": "A.",
"orcid": "0000-0002-1769-1640"
},
{
"family_name": "Dey",
"given_name": "A.",
"orcid": "0000-0002-4928-4003"
},
{
"family_name": "Dey",
"given_name": "B.",
"orcid": "0000-0002-5665-7912"
},
{
"family_name": "Doel",
"given_name": "P."
},
{
"family_name": "Fanning",
"given_name": "K.",
"orcid": "0000-0003-2371-3356"
},
{
"family_name": "Forero-Romero",
"given_name": "J. E.",
"orcid": "0000-0002-2890-3725"
},
{
"family_name": "Gazta\u00f1aga",
"given_name": "E.",
"orcid": "0000-0001-9632-0815"
},
{
"family_name": "Gontcho A Gontcho",
"given_name": "S.",
"orcid": "0000-0003-3142-233X"
},
{
"family_name": "Honscheid",
"given_name": "K."
},
{
"family_name": "Howlett",
"given_name": "C.",
"orcid": "0000-0002-1081-9410"
},
{
"family_name": "Kisner",
"given_name": "T.",
"orcid": "0000-0003-3510-7134"
},
{
"family_name": "Kremin",
"given_name": "A.",
"orcid": "0000-0001-6356-7424"
},
{
"family_name": "Lambert",
"given_name": "A.",
"orcid": "0009-0003-5658-2601"
},
{
"family_name": "Landriau",
"given_name": "M.",
"orcid": "0000-0003-1838-8528"
},
{
"family_name": "Le Guillou",
"given_name": "L.",
"orcid": "0000-0001-7178-8868"
},
{
"family_name": "Levi",
"given_name": "M. E.",
"orcid": "0000-0003-1887-1018"
},
{
"family_name": "Manera",
"given_name": "M.",
"orcid": "0000-0003-4962-8934"
},
{
"family_name": "Meisner",
"given_name": "A.",
"orcid": "0000-0002-1125-7384"
},
{
"family_name": "Miquel",
"given_name": "R."
},
{
"family_name": "Moustakas",
"given_name": "J.",
"orcid": "0000-0002-2733-4559"
},
{
"family_name": "Mueller",
"given_name": "E."
},
{
"family_name": "Myers",
"given_name": "A. D."
},
{
"family_name": "Nie",
"given_name": "J.",
"orcid": "0000-0001-6590-8122"
},
{
"family_name": "Palanque-Delabrouille",
"given_name": "N.",
"orcid": "0000-0003-3188-784X"
},
{
"family_name": "Poppett",
"given_name": "C."
},
{
"family_name": "Rezaie",
"given_name": "M.",
"orcid": "0000-0001-5589-7116"
},
{
"family_name": "Rossi",
"given_name": "G."
},
{
"family_name": "Sanchez",
"given_name": "E.",
"orcid": "0000-0002-9646-8198"
},
{
"family_name": "Schlegel",
"given_name": "D.",
"orcid": "0000-0002-5042-5088"
},
{
"family_name": "Schubnell",
"given_name": "M."
},
{
"family_name": "Seo",
"given_name": "H.",
"orcid": "0000-0002-6588-3508"
},
{
"family_name": "Sprayberry",
"given_name": "D."
},
{
"family_name": "Tarl\u00e9",
"given_name": "G.",
"orcid": "0000-0003-1704-0781"
},
{
"family_name": "Zou",
"given_name": "H.",
"orcid": "0000-0002-6684-3997"
}
],
"abstract": "Context. Gravitationally lensed type Ia supernovae (glSNe Ia) are unique astronomical tools that can be used to study cosmological parameters, distributions of dark matter, the astrophysics of the supernovae, and the intervening lensing galaxies themselves. A small number of highly magnified glSNe Ia have been discovered by ground-based telescopes such as the Zwicky Transient Facility (ZTF), but simulations predict that a fainter, undetected population may also exist.
\nAims. We present a systematic search for glSNe Ia in the ZTF archive of alerts distributed from June 1 2019 to September 1 2022.
\nMethods. Using the AMPEL platform, we developed a pipeline that distinguishes candidate glSNe Ia from other variable sources. Initial cuts were applied to the ZTF alert photometry (with constraints on the peak absolute magnitude and the distance to a catalogue-matched galaxy, as examples) before forced photometry was obtained for the remaining candidates. Additional cuts were applied to refine the candidates based on their light curve colours, lens galaxy colours, and the resulting parameters from fits to the SALT2 SN Ia template. The candidates were also cross-matched with the DESI spectroscopic catalogue.
\nResults. Seven transients were identified that passed all the cuts and had an associated galaxy DESI redshift, which we present as glSN Ia candidates. Although superluminous supernovae (SLSNe) cannot be fully rejected as contaminants, two events, ZTF19abpjicm and ZTF22aahmovu, are significantly different from typical SLSNe and their light curves can be modelled as two-image glSN Ia systems. From this two-image modelling, we estimate time delays of 22\u2005±\u20053 and 34\u2005±\u20051 days for the two events, respectively, which suggests that we have uncovered a population of glSNe Ia with longer time delays.
\nConclusions. The pipeline is efficient and sensitive enough to parse full alert streams. It is currently being applied to the live ZTF alert stream to identify and follow-up future candidates while active. This pipeline could be the foundation for glSNe Ia searches in future surveys, such as the Rubin Observatory Legacy Survey of Space and Time.
",
"doi": "10.1051/0004-6361/202451082",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A146"
},
{
"id": "authors:yffqt-jg984",
"collection": "authors",
"collection_id": "yffqt-jg984",
"cite_using_url": "https://authors.library.caltech.edu/records/yffqt-jg984",
"type": "article",
"title": "ZTF SN Ia DR2: Impact of the galaxy cluster environment on the stretch distribution of Type Ia supernovae",
"author": [
{
"family_name": "Ruppin",
"given_name": "F.",
"orcid": "0000-0002-0955-8954"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Ginolin",
"given_name": "M.",
"orcid": "0009-0004-5311-9301"
},
{
"family_name": "Dimitriadis",
"given_name": "G.",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Smith",
"given_name": "M.",
"orcid": "0000-0002-3321-1432"
},
{
"family_name": "Aubert",
"given_name": "M."
},
{
"family_name": "Biedermann",
"given_name": "J."
},
{
"family_name": "Copin",
"given_name": "Y.",
"orcid": "0000-0002-5317-7518"
},
{
"family_name": "Burgaz",
"given_name": "U.",
"orcid": "0000-0003-0126-3999"
},
{
"family_name": "Carreres",
"given_name": "B.",
"orcid": "0000-0002-7234-844X"
},
{
"family_name": "Feinstein",
"given_name": "F.",
"orcid": "0000-0001-5548-3466"
},
{
"family_name": "Fouchez",
"given_name": "D.",
"orcid": "0000-0002-7496-3796"
},
{
"family_name": "Muller-Bravo",
"given_name": "T. E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Galbany",
"given_name": "L.",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Kenworthy",
"given_name": "W. D.",
"orcid": "0000-0002-5153-5983"
},
{
"family_name": "Kim",
"given_name": "Y. -L.",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Nugent",
"given_name": "P.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Popovic",
"given_name": "B.",
"orcid": "0000-0002-8012-6978"
},
{
"family_name": "Purdum",
"given_name": "J.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Racine",
"given_name": "B.",
"orcid": "0000-0001-8861-3052"
},
{
"family_name": "Rosnet",
"given_name": "P.",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Rosselli",
"given_name": "D.",
"orcid": "0000-0001-6839-1421"
},
{
"family_name": "Smith",
"given_name": "R.",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-Roger"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Terwel",
"given_name": "J. H.",
"orcid": "0000-0001-9834-3439"
}
],
"abstract": "Context. Understanding the impact of the astrophysical environment on Type Ia supernova (SN Ia) properties is crucial to minimize systematic uncertainties in cosmological analyses based on this probe.
\nAims. We investigate the dependence of the SN Ia SALT2.4 light-curve stretch on the distance from their nearest galaxy cluster to study the potential effect of the intracluster medium (ICM) environment on the intrinsic properties of SN Ia.
\nMethods. We used the largest SN Ia sample to date and cross-matched it with existing X-ray, Sunyaev–Zel'dovich, and optical cluster catalogs in order to study the relation between the stretch and the distance to the nearest detected cluster from each SN Ia. We modeled the underlying stretch distribution with a Gaussian mixture with relative amplitudes that depended on redshift and clustercentric distance.
\nResults. We find that the fit quality of the stretch distribution improves significantly when we included the distance-dependant term in the model with a variation of the Akaike information criterion ΔAIC\u2004=\u2004−10.2. Because of the known correlation between galaxy age and distance from the cluster center, this supports previous evidence that the age of the stellar population is the underlying driver of the bimodal shape of the SN Ia stretch distribution. We further computed the evolution of the fraction of quenched galaxies as a function of distance with respect to cluster center from our best-fit model of the SNe Ia stretch distribution and compared it to previous results obtained from Hα line measurements, optical broadband photometry, and simulations. We find our estimate to be compatible with these results.
\nConclusions. The results of this work indicate that SNe Ia searches at high redshift targeted toward clusters to maximize detection probability should be considered with caution as the stretch distribution of the detected sample would be strongly biased toward the old subpopulation of SNe Ia. Furthermore, the effect of the ICM environment on the SN Ia properties appears to be significant from the center of the clusters up to their splashback radius. This is compatible with previous works based on observations and simulations of a galaxy age gradient with respect to clustercentric distance in massive cluster halos. The next generation of large-area surveys will provide an increase of an order of magnitude in the size of SN Ia and cluster catalogs. This will enable us to analyze the impact of cluster mass on the intrinsic properties of SNe Ia and of the fraction of quenched galaxies in the outskirts of clusters in more detail, where direct measurements are challenging.
",
"doi": "10.1051/0004-6361/202450956",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A6"
},
{
"id": "authors:dyw1w-j3380",
"collection": "authors",
"collection_id": "dyw1w-j3380",
"cite_using_url": "https://authors.library.caltech.edu/records/dyw1w-j3380",
"type": "article",
"title": "ZTF SN Ia DR2: Simulations and volume-limited sample",
"author": [
{
"family_name": "Amenouche",
"given_name": "M.",
"orcid": "0009-0006-7454-3579"
},
{
"family_name": "Rosnet",
"given_name": "P.",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Smith",
"given_name": "M.",
"orcid": "0000-0002-3321-1432"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Aubert",
"given_name": "M.",
"orcid": "0009-0002-7667-8814"
},
{
"family_name": "Barjou-Delayre",
"given_name": "C."
},
{
"family_name": "Burgaz",
"given_name": "U.",
"orcid": "0000-0003-0126-3999"
},
{
"family_name": "Carreres",
"given_name": "B.",
"orcid": "0000-0002-7234-844X"
},
{
"family_name": "Dimitriadis",
"given_name": "G.",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Feinstein",
"given_name": "F.",
"orcid": "0000-0001-5548-3466"
},
{
"family_name": "Galbany",
"given_name": "L.",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Ginolin",
"given_name": "M.",
"orcid": "0009-0004-5311-9301"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Harvey",
"given_name": "L.",
"orcid": "0000-0003-3393-9383"
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Kim",
"given_name": "Y.-L.",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "T. E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Nugent",
"given_name": "P.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Racine",
"given_name": "B.",
"orcid": "0000-0001-8861-3052"
},
{
"family_name": "Rosselli",
"given_name": "D.",
"orcid": "0000-0001-6839-1421"
},
{
"family_name": "Regnault",
"given_name": "N.",
"orcid": "0000-0001-7029-7901"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Terwel",
"given_name": "J. H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Townsend",
"given_name": "A.",
"orcid": "0000-0001-6343-3362"
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kasliwal",
"given_name": "M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Purdum",
"given_name": "J.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
}
],
"abstract": "Type Ia supernovae (SNe Ia) constitute a historical probe for deriving cosmological parameters through the fit of the Hubble-Lema\u00eetre diagram, that is, the SN Ia distance modulus versus their redshift. In the era of precision cosmology, realistic simulation of SNe Ia for any survey entering an Hubble-Lema\u00eetre diagram is a key tool for addressing observational systematics, such as the Malmquist bias. As the distance modulus of SNe Ia is derived from the fit of their light curves, a robust simulation framework is required. In this paper, we present the performances of the simulation framework skysurvey with the aim to reproduce the Zwicky Transient Facility (ZTF) SN Ia DR2, which covers the first phase of the ZTF and ran from March 2018 to December 2020. The ZTF SN Ia DR2 sample corresponds to almost 3000 classified SNe Ia of cosmological quality. We simulated individual light curves of the ZTF SN Ia DR2 sample to confirm the validity of the framework while taking the observing conditions and instrument performances into account. After the ZTF SN Ia DR2 selection criteria were applied, we found that the simulated fluxes and associated uncertainties agre well with the measured uncertainties when the sky-noise deduced from the observed science magnitude limits is corrected for by a factor 1.23 for the g band, 1.17 for the r band, and 1.20 for the i band. In addition, we accounted for an error floor of 2.5%, 3.5%, and 6% of the flux level in the g, r, and i bands, respectively. Furthermore a redshift dependence of the SALT2 light-curve parameters (stretch and colour) was conducted to deduce the redshift limit that defines a volume-limited sample, that is, an unbiased SNe Ia sample. We found that the ZTF SN Ia DR2 volume-limited sample is characterized by z\u2004\u2264\u20040.06. This volume-limited sample of about 1000 SNe Ia is unique, and an astrophysical analysis can be carried out based on it, or the standardisation procedure can be tested with unprecedented precision (these analyses are presented in companion papers).",
"doi": "10.1051/0004-6361/202452134",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A3"
},
{
"id": "authors:kbzzf-qxj09",
"collection": "authors",
"collection_id": "kbzzf-qxj09",
"cite_using_url": "https://authors.library.caltech.edu/records/kbzzf-qxj09",
"type": "article",
"title": "ZTF SN Ia DR2: Searching for late-time interaction signatures in Type Ia supernovae from the Zwicky Transient Facility",
"author": [
{
"family_name": "Terwel",
"given_name": "Jacco H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Maguire",
"given_name": "Kate",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Dimitriadis",
"given_name": "Georgios",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Smith",
"given_name": "Mat",
"orcid": "0000-0002-3321-1432"
},
{
"family_name": "Reusch",
"given_name": "Simeon",
"orcid": "0000-0002-7788-628X"
},
{
"family_name": "Lacroix",
"given_name": "Leander",
"orcid": "0000-0003-0629-5746"
},
{
"family_name": "Galbany",
"given_name": "Llu\u00eds",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Burgaz",
"given_name": "Umut",
"orcid": "0000-0003-0126-3999"
},
{
"family_name": "Harvey",
"given_name": "Luke",
"orcid": "0000-0003-3393-9383"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-David"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kim",
"given_name": "Young-Lo",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Anderson",
"given_name": "Joseph P.",
"orcid": "0000-0003-0227-3451"
},
{
"family_name": "Chen",
"given_name": "Ting-Wan",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Frohmaier",
"given_name": "Christopher",
"orcid": "0000-0001-9553-4723"
},
{
"family_name": "Gromadzki",
"given_name": "Mariusz",
"orcid": "0000-0002-1650-1518"
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "Tom\u00e1s E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Srivastav",
"given_name": "Shubham",
"orcid": "0000-0003-4524-6883"
},
{
"family_name": "Deckers",
"given_name": "Maxime",
"orcid": "0000-0001-8857-9843"
}
],
"abstract": "The nature of the progenitor systems and explosion mechanisms that give rise to Type Ia supernovae (SNe Ia) are still debated. The interaction signature of circumstellar material (CSM) being swept up by the expanding ejecta can constrain the type of system from which it was ejected. However, most previous studies have focussed on finding CSM ejected shortly before the SN Ia explosion, which still resides close to the explosion site resulting in short delay times until the interaction starts. We used a sample of 3628 SNe Ia from the Zwicky Transient Facility (ZTF) that were discovered between 2018 and 2020 and searched for interaction signatures greater than 100 days after peak brightness. By binning the late-time light curve data to push the detection limit as deep as possible, we identified potential late-time rebrightening in three SNe Ia (SN 2018grt, SN 2019dlf, and SN 2020tfc). The late-time optical detections occur between 550 and 1450 d after peak brightness, have mean absolute r-band magnitudes of −16.4 to −16.8 mag, and last up to a few hundred days, which is significantly brighter than the late-time CSM interaction discovered in the prototype, SN 2015cp. The late-time detections in the three objects all occur within 0.8 kpc of the host nucleus and are not easily explained by nuclear activity, another transient at a similar sky position, or data quality issues. This is suggestive of environment or specific progenitor characteristics playing a role in the production of potential CSM signatures in these SNe Ia. Through simulating the ZTF survey, we estimate that < 0.5% of normal SNe Ia display a late-time (> 100 d post peak) strong Hα-dominated CSM interaction. This is equivalent to an absolute rate of 8−4+20 to 54−26+91 Gpc−3 yr−1 assuming a constant SN Ia rate of 2.4\u2005×\u200510−5 Mpc−3 yr−1 for z\u2004≤\u20040.1. Weaker interaction signatures of Hα emission, more similar to the strength seen in SN 2015cp, could be more common but are difficult to constrain with our survey depth.
",
"doi": "10.1051/0004-6361/202348476",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A11"
},
{
"id": "authors:frc4j-4a782",
"collection": "authors",
"collection_id": "frc4j-4a782",
"cite_using_url": "https://authors.library.caltech.edu/records/frc4j-4a782",
"type": "article",
"title": "ZTF SN Ia DR2: Peculiar velocities' impact on the Hubble diagram",
"author": [
{
"family_name": "Carreres",
"given_name": "B.",
"orcid": "0000-0002-7234-844X"
},
{
"family_name": "Rosselli",
"given_name": "D.",
"orcid": "0000-0001-6839-1421"
},
{
"family_name": "Bautista",
"given_name": "J. E.",
"orcid": "0000-0002-9885-3989"
},
{
"family_name": "Feinstein",
"given_name": "F.",
"orcid": "0000-0001-5548-3466"
},
{
"family_name": "Fouchez",
"given_name": "D.",
"orcid": "0000-0002-7496-3796"
},
{
"family_name": "Racine",
"given_name": "B.",
"orcid": "0000-0001-8861-3052"
},
{
"family_name": "Ravoux",
"given_name": "C.",
"orcid": "0000-0002-3500-6635"
},
{
"family_name": "Sanchez",
"given_name": "B."
},
{
"family_name": "Dimitriadis",
"given_name": "G.",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Goobar",
"given_name": "A."
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Smith",
"given_name": "M.",
"orcid": "0000-0002-3321-1432"
},
{
"family_name": "Amenouche",
"given_name": "M.",
"orcid": "0009-0006-7454-3579"
},
{
"family_name": "Aubert",
"given_name": "M.",
"orcid": "0009-0002-7667-8814"
},
{
"family_name": "Barjou-Delayre",
"given_name": "C."
},
{
"family_name": "Burgaz",
"given_name": "U.",
"orcid": "0000-0003-0126-3999"
},
{
"family_name": "D'Arcy Kenworthy",
"given_name": "W.",
"orcid": "0000-0002-5153-5983"
},
{
"family_name": "De Jaeger",
"given_name": "T."
},
{
"family_name": "Dhawan",
"given_name": "S.",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Galbany",
"given_name": "L.",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Ginolin",
"given_name": "M.",
"orcid": "0009-0004-5311-9301"
},
{
"family_name": "Kuhn",
"given_name": "D.",
"orcid": "0009-0005-8110-397X"
},
{
"family_name": "Kowalski",
"given_name": "M.",
"orcid": "0000-0001-8594-8666"
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "T. E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Nugent",
"given_name": "P. E.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Popovic",
"given_name": "B."
},
{
"family_name": "Rosnet",
"given_name": "P.",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Ruppin",
"given_name": "F."
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Terwel",
"given_name": "J. H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Townsend",
"given_name": "A.",
"orcid": "0000-0001-6343-3362"
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Purdum",
"given_name": "J.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sravan",
"given_name": "N."
}
],
"abstract": "Type Ia supernovae (SNe Ia) are used to determine the distance-redshift relation and build the Hubble diagram. Neglecting their host-galaxy peculiar velocities (PVs) may bias the measurement of cosmological parameters. The smaller the redshift, the larger the effect is. We used realistic simulations of SNe Ia observed by the Zwicky Transient Facility (ZTF) to investigate the effect of different methods of taking PVs into account. We studied the impact of neglecting galaxy PVs and their correlations in an analysis of the SNe Ia Hubble diagram. We find that it is necessary to use the PV full covariance matrix computed from the velocity power spectrum to take the sample variance into account. Considering the results we have obtained using simulations, we determine the PV systematic effects in the context of the ZTF SN Ia DR2 sample. We determine the PV impact on the intercept of the Hubble diagram, aB, which is directly linked to the measurement of H0. We show that not taking into account PVs and their correlations results in a shift in the H0 value of about 1.0 km s−1 Mpc−1 and a slight underestimation of the H0 error bar.
",
"doi": "10.1051/0004-6361/202450389",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A8"
},
{
"id": "authors:8wz9z-8yg11",
"collection": "authors",
"collection_id": "8wz9z-8yg11",
"cite_using_url": "https://authors.library.caltech.edu/records/8wz9z-8yg11",
"type": "article",
"title": "ZTF SN Ia DR2: The diversity and relative rates of the thermonuclear supernova population",
"author": [
{
"family_name": "Dimitriadis",
"given_name": "G.",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Burgaz",
"given_name": "U.",
"orcid": "0000-0003-0126-3999"
},
{
"family_name": "Deckers",
"given_name": "M.",
"orcid": "0000-0001-8857-9843"
},
{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Smith",
"given_name": "M.",
"orcid": "0000-0002-3321-1432"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Frohmaier",
"given_name": "C.",
"orcid": "0000-0001-9553-4723"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Galbany",
"given_name": "L.",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Kim",
"given_name": "Y.-L.",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Liu",
"given_name": "C.",
"orcid": "0000-0002-7866-4531"
},
{
"family_name": "Miller",
"given_name": "A. A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Nugent",
"given_name": "P. E.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Alburai",
"given_name": "A.",
"orcid": "0009-0007-2731-5562"
},
{
"family_name": "Chen",
"given_name": "P.",
"orcid": "0000-0003-0853-6427"
},
{
"family_name": "Dhawan",
"given_name": "S.",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Ginolin",
"given_name": "M.",
"orcid": "0009-0004-5311-9301"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Harvey",
"given_name": "L.",
"orcid": "0000-0003-3393-9383"
},
{
"family_name": "Kenworthy",
"given_name": "W. D.",
"orcid": "0000-0002-5153-5983"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Phan",
"given_name": "K.",
"orcid": "0000-0001-6383-860X"
},
{
"family_name": "Popovic",
"given_name": "B.",
"orcid": "0000-0002-8012-6978"
},
{
"family_name": "Riddle",
"given_name": "R. L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "T. E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Terwel",
"given_name": "J. H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Townsend",
"given_name": "A.",
"orcid": "0000-0001-6343-3362"
}
],
"abstract": "The Zwicky Transient Facility SN Ia Data Release 2 (ZTF SN Ia DR2) contains more than 3000 Type Ia supernovae (SNe Ia), providing the largest homogeneous low-redshift sample of SNe Ia. Having at least one spectrum per event, this data collection is ideal for large-scale statistical studies of the photometric, spectroscopic and host-galaxy properties of SNe Ia, particularly of the rarer 'peculiar' sub-classes. In this paper we first present the method we developed to spectroscopically classify the SNe in the sample, and the techniques we used to model their multi-band light curves and explore their photometric properties. We then show a method to distinguish between the peculiar sub-types and the normal SNe Ia. We also explore the properties of their host galaxies and estimate their relative rates, focusing on the peculiar sub-types and their connection to the cosmologically useful SNe Ia. Finally, we discuss the implications of our study with respect to the progenitor systems of the peculiar SN Ia events.",
"doi": "10.1051/0004-6361/202451852",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A10"
},
{
"id": "authors:qz82n-mwq18",
"collection": "authors",
"collection_id": "qz82n-mwq18",
"cite_using_url": "https://authors.library.caltech.edu/records/qz82n-mwq18",
"type": "article",
"title": "ZTF SN Ia DR2: Overview",
"author": [
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Smith",
"given_name": "M.",
"orcid": "0000-0002-3321-1432"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Dimitriadis",
"given_name": "G.",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Burgaz",
"given_name": "U.",
"orcid": "0000-0003-0126-3999"
},
{
"family_name": "Dhawan",
"given_name": "S.",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Regnault",
"given_name": "N.",
"orcid": "0000-0001-7029-7901"
},
{
"family_name": "Kowalski",
"given_name": "M.",
"orcid": "0000-0001-8594-8666"
},
{
"family_name": "Nugent",
"given_name": "P.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Amenouche",
"given_name": "M.",
"orcid": "0009-0006-7454-3579"
},
{
"family_name": "Aubert",
"given_name": "M."
},
{
"family_name": "Barjou-Delayre",
"given_name": "C."
},
{
"family_name": "Bautista",
"given_name": "J.",
"orcid": "0000-0002-9885-3989"
},
{
"family_name": "Bellm",
"given_name": "E.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Betoule",
"given_name": "M.",
"orcid": "0000-0003-0804-836X"
},
{
"family_name": "Bloom",
"given_name": "J. S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Carreres",
"given_name": "B.",
"orcid": "0000-0002-7234-844X"
},
{
"family_name": "Chen",
"given_name": "T. X.",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-X"
},
{
"family_name": "Copin",
"given_name": "Y.",
"orcid": "0000-0002-5317-7518"
},
{
"family_name": "Deckers",
"given_name": "M.",
"orcid": "0000-0001-8857-9843"
},
{
"family_name": "de Jaeger",
"given_name": "T.",
"orcid": "0000-0001-6069-1139"
},
{
"family_name": "Feinstein",
"given_name": "F.",
"orcid": "0000-0001-5548-3466"
},
{
"family_name": "Fouchez",
"given_name": "D.",
"orcid": "0000-0002-7496-3796"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Galbany",
"given_name": "L.",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Ginolin",
"given_name": "M.",
"orcid": "0009-0004-5311-9301"
},
{
"family_name": "Graham",
"given_name": "M.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Harvey",
"given_name": "L.",
"orcid": "0000-0003-3393-9383"
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{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
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{
"family_name": "Kenworthy",
"given_name": "W. D.",
"orcid": "0000-0002-5153-5983"
},
{
"family_name": "Kim",
"given_name": "Y.-L.",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Kuhn",
"given_name": "D.",
"orcid": "0009-0005-8110-397X"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Lacroix",
"given_name": "L.",
"orcid": "0000-0003-0629-5746"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "T. E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Miller",
"given_name": "A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Osman",
"given_name": "M.",
"orcid": "0009-0000-6101-6725"
},
{
"family_name": "Perley",
"given_name": "D.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Popovic",
"given_name": "B.",
"orcid": "0000-0002-8012-6978"
},
{
"family_name": "Purdum",
"given_name": "J.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Qin",
"given_name": "Y.-J.",
"orcid": "0000-0003-3658-6026",
"clpid": "Qin-Yu-Jing"
},
{
"family_name": "Racine",
"given_name": "B.",
"orcid": "0000-0001-8861-3052"
},
{
"family_name": "Reusch",
"given_name": "S.",
"orcid": "0000-0002-7788-628X"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Rosnet",
"given_name": "P.",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Rosselli",
"given_name": "D.",
"orcid": "0000-0001-6839-1421"
},
{
"family_name": "Ruppin",
"given_name": "F.",
"orcid": "0000-0002-0955-8954"
},
{
"family_name": "Senzel",
"given_name": "R.",
"orcid": "0009-0002-0243-8199"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Schweyer",
"given_name": "T.",
"orcid": "0000-0001-8948-3456"
},
{
"family_name": "Terwel",
"given_name": "J. H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Townsend",
"given_name": "A.",
"orcid": "0000-0001-6343-3362"
},
{
"family_name": "Tzanidakis",
"given_name": "A.",
"orcid": "0000-0003-0484-3331"
},
{
"family_name": "Wold",
"given_name": "A.",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We present the first homogeneous release of several thousand spectroscopically classified type Ia supernovae (SNe Ia) with spectroscopic redshifts. This release, named “DR2”, contains 3628 nearby (z\u2004<\u20040.3) SNe Ia discovered, followed, and classified by the Zwicky Transient Facility survey between March 2018 and December 2020. Of these, 3000 have good-to-excellent sampling and 2667 pass standard cosmology light curve quality cuts. This release is thus the largest SN Ia release to date, increasing by an order of magnitude the number of well-characterized low-redshift objects. With DR2, we also provide a volume-limited (z\u2004<\u20040.06) sample of nearly a thousand SNe Ia. With such a large, homogeneous, and well-controlled dataset, we are studying key current questions on SN cosmology, such as the linearity SNe Ia standardization, the SN and host dependencies, the diversity of the SN Ia population, and the accuracy of current light curve modeling. These, and more, are studied in detail in a series of articles associated with this release. Alongside the SN Ia parameters, we publish our forced-photometry gri-band light curves, 5138 spectra, local and global host properties, observing logs, and a Python tool to facilitate the use and access of these data. The photometric accuracy of DR2 is not yet suited for cosmological parameter inference, which will follow as the “DR2.5” release. We nonetheless demonstrate that our Hubble diagram of several thousands of SNe Ia has a typical 0.15 mag scatter.
",
"doi": "10.1051/0004-6361/202450388",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A1"
},
{
"id": "authors:0smha-tck25",
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"collection_id": "0smha-tck25",
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"type": "article",
"title": "Cataclysmic Variables and AM CVn Binaries in SRG/eROSITA + Gaia: Volume Limited Samples, X-Ray Luminosity Functions, and Space Densities",
"author": [
{
"family_name": "Rodriguez",
"given_name": "Antonio C.",
"orcid": "0000-0003-4189-9668",
"clpid": "Rodriguez-Antonio-C"
},
{
"family_name": "El-Badry",
"given_name": "Kareem",
"orcid": "0000-0002-6871-1752",
"clpid": "El-Badry-Kareem"
},
{
"family_name": "Suleimanov",
"given_name": "Valery",
"orcid": "0000-0003-3733-7267"
},
{
"family_name": "Pala",
"given_name": "Anna F.",
"orcid": "0000-0001-7069-7403"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Gaensicke",
"given_name": "Boris",
"orcid": "0000-0002-2761-3005"
},
{
"family_name": "Mori",
"given_name": "Kaya",
"orcid": "0000-0002-9709-5389"
},
{
"family_name": "Rich",
"given_name": "R. Michael",
"orcid": "0000-0003-0427-8387"
},
{
"family_name": "Sarkar",
"given_name": "Arnab",
"orcid": "0000-0002-1455-2784"
},
{
"family_name": "Bao",
"given_name": "Tong",
"orcid": "0000-0002-5082-5049"
},
{
"family_name": "de Oliveira",
"given_name": "Raimundo Lopes",
"orcid": "0000-0002-6211-7226"
},
{
"family_name": "Ramsay",
"given_name": "Gavin",
"orcid": "0000-0001-8722-9710"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"orcid": "0000-0003-4373-7777"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Caiazzo",
"given_name": "Ilaria",
"orcid": "0000-0002-4770-5388",
"clpid": "Caiazzo-Ilaria"
},
{
"family_name": "Vanderbosch",
"given_name": "Zachary P.",
"orcid": "0000-0002-0853-3464",
"clpid": "Vanderbosch-Zachary-P"
},
{
"family_name": "Roestel",
"given_name": "Jan van",
"orcid": "0000-0002-2626-2872"
},
{
"family_name": "Das",
"given_name": "Kaustav K.",
"orcid": "0000-0001-8372-997X",
"clpid": "Das-Kaustav-K"
},
{
"family_name": "Qin",
"given_name": "Yu-Jing",
"orcid": "0000-0003-3658-6026",
"clpid": "Qin-Yu-Jing"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Reiley",
"given_name": "Daniel",
"clpid": "Reiley-Daniel"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
}
],
"abstract": "We present volume-limited samples of cataclysmic variables (CVs) and AM CVn binaries jointly selected from SRG/eROSITA eRASS1 and Gaia DR3 using an X-ray + optical color–color diagram (the “X-ray Main Sequence”). This tool identifies all CV subtypes, including magnetic and low-accretion rate systems, in contrast to most previous surveys. We find 23 CVs, 3 of which are AM CVns, out to 150 pc in the Western Galactic Hemisphere. Our 150 pc sample is spectroscopically verified and complete down to LX = 1.3 × 1029 erg s−1 in the 0.2–2.3 keV band, and we also present CV candidates out to 300 pc and 1000 pc. We discovered two previously unknown systems in our 150 pc sample: the third nearest AM CVn and a magnetic period bouncer. We find the mean LX of CVs to be \u3008LX\u3009 ≈ 4.6 × 1030 erg s−1, in contrast to previous surveys which yielded \u3008LX\u3009 ∼ 1031−1032 erg s−1. We construct X-ray luminosity functions that, for the first time, flatten out at LX ∼ 1030 erg s−1. We infer average number, mass, and luminosity densities of ρN,CV = (3.7 ± 0.7) × 10−6pc−3, ρM = (5.0 ± 1.0) ×10−\u2075 M \u2299−1, and ρLX = (2.3 ± 0.4) × 10²\u2076 erg s−1M\u2299−1, respectively, in the solar neighborhood. Our uniform selection method also allows us to place meaningful estimates on the space density of AM CVns, ρN,AM CVn = (5.5 ± 3.7) × 10−7 pc−3. Magnetic CVs and period bouncers make up 35% and 25% of our sample, respectively. This work, through a novel discovery technique, shows that the observed number densities of CVs and AM CVns, as well as the fraction of period bouncers, are still in tension with population synthesis estimates.
",
"doi": "10.1088/1538-3873/ada185",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2025-01",
"series_number": "1",
"volume": "137",
"issue": "1",
"pages": "014201"
},
{
"id": "authors:fs2dx-ay491",
"collection": "authors",
"collection_id": "fs2dx-ay491",
"cite_using_url": "https://authors.library.caltech.edu/records/fs2dx-ay491",
"type": "article",
"title": "Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility",
"author": [
{
"family_name": "Srinivasaragavan",
"given_name": "Gokul P.",
"orcid": "0000-0002-6428-2700"
},
{
"family_name": "Yang",
"given_name": "Sheng",
"orcid": "0000-0002-2898-6532"
},
{
"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"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Corsi",
"given_name": "Alessandra",
"orcid": "0000-0001-8104-3536"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Perley",
"given_name": "Daniel",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Sanchez-Fleming",
"given_name": "Marquice",
"orcid": "0009-0002-0416-841X"
},
{
"family_name": "Pope",
"given_name": "Jack"
},
{
"family_name": "Sarin",
"given_name": "Nikhil",
"orcid": "0000-0003-2700-1030"
},
{
"family_name": "Omand",
"given_name": "Conor",
"orcid": "0000-0002-9646-8710"
},
{
"family_name": "Das",
"given_name": "Kaustav K.",
"orcid": "0000-0001-8372-997X",
"clpid": "Das-Kaustav-K"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Bruch",
"given_name": "Rachel",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"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": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007"
},
{
"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": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Martikainen",
"given_name": "Julia",
"orcid": "0000-0003-2211-4001"
},
{
"family_name": "Sharma",
"given_name": "Yashvi S.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi-S"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331"
},
{
"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"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank"
},
{
"family_name": "Nir",
"given_name": "Guy",
"orcid": "0000-0002-7501-5579"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Sravan",
"given_name": "Niharika"
}
],
"abstract": "We study a magnitude-limited sample of 36 broad-lined type Ic supernovae (SNe Ic-BL) from the Zwicky Transient Facility Bright Transient Survey (detected between 2018 March and 2021 August), which is the largest systematic study of SNe Ic-BL done in literature thus far. We present the light curves (LCs) for each of the SNe and analyze the shape of the LCs to derive empirical parameters, along with the explosion epochs for every event. The sample has an average absolute peak magnitude in the r band of M_(r, max) = −18.51 ± 0.15 mag. Using spectra obtained around peak light, we compute expansion velocities from the Fe ii 5169 Å line for each event with high enough signal-to-noise ratio spectra, and find an average value of v_(ph) = 16,100 ± 1100 km s\u207b¹. We also compute bolometric LCs, study the blackbody temperature and radii evolution over time, and derive the explosion properties of the SNe. The explosion properties of the sample have average values of M(Ni) = 0.37_(−0.06)^(+0.08) M\u2299, M_(ej) = 2.45_(−0.41)^(+0.47) M\u2299, and E_K = (4.02_(−1.00)^(+1.37) × 10\u2075¹ erg. Thirteen events have radio observations from the Very Large Array, with eight detections and five non-detections. We find that the populations that have radio detections and radio non-detections are indistinct from one another with respect to their optically inferred explosion properties, and there are no statistically significant correlations present between the events' radio luminosities and optically inferred explosion properties. This provides evidence that the explosion properties derived from optical data alone cannot give inferences about the radio properties of SNe Ic-BL and likely their relativistic jet formation mechanisms.
",
"doi": "10.3847/1538-4357/ad7fde",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2024-11-20",
"series_number": "1",
"volume": "976",
"issue": "1",
"pages": "71"
},
{
"id": "authors:4881f-cag42",
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"collection_id": "4881f-cag42",
"cite_using_url": "https://authors.library.caltech.edu/records/4881f-cag42",
"type": "article",
"title": "Probing Presupernova Mass Loss in Double-peaked Type Ibc Supernovae from the Zwicky Transient Facility",
"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": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Irani",
"given_name": "I.",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Leung",
"given_name": "Shing-Chi",
"orcid": "0000-0002-4972-3803"
},
{
"family_name": "Wu",
"given_name": "Samantha",
"orcid": "0000-0003-2872-5153",
"clpid": "Wu-Samantha"
},
{
"family_name": "Fuller",
"given_name": "Jim",
"orcid": "0000-0002-4544-0750",
"clpid": "Fuller-J"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Barbarino",
"given_name": "C.",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Dugas",
"given_name": "Alison"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Hinds",
"given_name": "K-Ryan",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Regnault",
"given_name": "Nicolas"
},
{
"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": "Sit",
"given_name": "Tawny",
"orcid": "0000-0001-8208-9755"
},
{
"family_name": "Sravan",
"given_name": "Niharika"
},
{
"family_name": "Srinivasaragavan",
"given_name": "Gokul P.",
"orcid": "0000-0002-6428-2700"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Tartaglia",
"given_name": "Leonardo",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"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": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Zolkower",
"given_name": "Jeffry",
"clpid": "Zolkower-Jeffry"
}
],
"abstract": "\n
Eruptive mass loss of massive stars prior to supernova (SN) explosion is key to understanding their evolution and end fate. An observational signature of pre-SN mass loss is the detection of an early, short-lived peak prior to the radioactive-powered peak in the lightcurve of the SN. This is usually attributed to the SN shock passing through an extended envelope or circumstellar medium. Such an early peak is common for double-peaked Type IIb SNe with an extended hydrogen envelope but uncommon for normal Type Ibc SNe with very compact progenitors. In this paper, we systematically study a sample of 14 double-peaked Type Ibc SNe out of 475 Type Ibc SNe detected by the Zwicky Transient Facility. The rate of these events is ∼3%–9% of Type Ibc SNe. A strong correlation is seen between the peak brightness of the first and the second peak. We perform a holistic analysis of this sample’s photometric and spectroscopic properties. We find that six SNe have ejecta mass less than 1.5 M\u2299. Based on the nebular spectra and lightcurve properties, we estimate that the progenitor masses for these are less than ∼12 M\u2299. The rest have an ejecta mass >2.4 M\u2299 and a higher progenitor mass. This sample suggests that the SNe with low progenitor masses undergo late-time binary mass transfer. Meanwhile, the SNe with higher progenitor masses are consistent with wave-driven mass loss or pulsation-pair instability-driven mass-loss simulations.
\n
Stars with zero-age main sequence masses between 140 and 260\u2006M\u2299 are thought to explode as pair-instability supernovae (PISNe). During their thermonuclear runaway, PISNe can produce up to several tens of solar masses of radioactive nickel, resulting in luminous transients similar to some superluminous supernovae (SLSNe). Yet, no unambiguous PISN has been discovered so far. SN 2018ibb is a hydrogen-poor SLSN at z\u2004=\u20040.166 that evolves extremely slowly compared to the hundreds of known SLSNe. Between mid 2018 and early 2022, we monitored its photometric and spectroscopic evolution from the UV to the near-infrared (NIR) with 2–10 m class telescopes. SN 2018ibb radiated > 3\u2005×\u20051051\u2006erg during its evolution, and its bolometric light curve reached > 2\u2005×\u20051044\u2006erg\u2006s−1 at its peak. The long-lasting rise of > 93 rest-frame days implies a long diffusion time, which requires a very high total ejected mass. The PISN mechanism naturally provides both the energy source (56Ni) and the long diffusion time. Theoretical models of PISNe make clear predictions as to their photometric and spectroscopic properties. SN 2018ibb complies with most tests on the light curves, nebular spectra and host galaxy, and potentially all tests with the interpretation we propose. Both the light curve and the spectra require 25–44 M\u2299 of freshly nucleosynthesised 56Ni, pointing to the explosion of a metal-poor star with a helium core mass of 120–130 M\u2299 at the time of death. This interpretation is also supported by the tentative detection of [Co\u202fII] λ 1.025 μm, which has never been observed in any other PISN candidate or SLSN before. We observe a significant excess in the blue part of the optical spectrum during the nebular phase, which is in tension with predictions of existing PISN models. However, we have compelling observational evidence for an eruptive mass-loss episode of the progenitor of SN 2018ibb shortly before the explosion, and our dataset reveals that the interaction of the SN ejecta with this oxygen-rich circumstellar material contributed to the observed emission. That may explain this specific discrepancy with PISN models. Powering by a central engine, such as a magnetar or a black hole, can be excluded with high confidence. This makes SN 2018ibb by far the best candidate for being a PISN, to date.
",
"doi": "10.1051/0004-6361/202346855",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2024-03",
"volume": "683",
"pages": "A223"
},
{
"id": "authors:30yrb-yt749",
"collection": "authors",
"collection_id": "30yrb-yt749",
"cite_using_url": "https://authors.library.caltech.edu/records/30yrb-yt749",
"type": "article",
"title": "A 12.4-day periodicity in a close binary system after a supernova",
"author": [
{
"family_name": "Chen",
"given_name": "Ping",
"orcid": "0000-0003-0853-6427",
"clpid": "Chen-Ping"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Post",
"given_name": "Richard S.",
"orcid": "0000-0003-3244-0337"
},
{
"family_name": "Liu",
"given_name": "Chang",
"orcid": "0000-0002-7866-4531"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Das",
"given_name": "Kaustav K.",
"clpid": "Das-Kaustav-K"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Horesh",
"given_name": "Assaf",
"orcid": "0000-0002-5936-1156"
},
{
"family_name": "Katz",
"given_name": "Boaz",
"orcid": "0000-0003-0584-2920"
},
{
"family_name": "Kushnir",
"given_name": "Doron"
},
{
"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": "Liu",
"given_name": "Dezi",
"orcid": "0000-0002-0409-5719"
},
{
"family_name": "Liu",
"given_name": "Xiangkun",
"orcid": "0000-0003-0394-1298"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Rose",
"given_name": "Kovi",
"orcid": "0000-0002-7329-3209"
},
{
"family_name": "Waxman",
"given_name": "Eli",
"orcid": "0000-0002-9038-5877"
},
{
"family_name": "Yang",
"given_name": "Sheng",
"orcid": "0000-0002-2898-6532"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Zackay",
"given_name": "Barak",
"clpid": "Zackay-Barak"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Fang",
"given_name": "Yuan"
},
{
"family_name": "Fynbo",
"given_name": "Johan P. U.",
"orcid": "0000-0002-8149-8298"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Jegou du Laz",
"given_name": "Theophile",
"orcid": "0009-0003-6181-4526",
"clpid": "Jegou-du-Laz-Theophile"
},
{
"family_name": "Liu",
"given_name": "Xiaowei"
},
{
"family_name": "Mazzali",
"given_name": "Paolo A.",
"orcid": "0000-0001-6876-8284"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Qin",
"given_name": "Yu-Jing",
"orcid": "0000-0003-3658-6026",
"clpid": "Qin-Yu-Jing"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X"
},
{
"family_name": "Sharon",
"given_name": "Amir",
"orcid": "0009-0000-2102-5811"
},
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730"
},
{
"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"
}
],
"abstract": "\n
\n
Neutron stars and stellar-mass black holes are the remnants of massive star explosions1. Most massive stars reside in close binary systems2, and the interplay between the companion star and the newly formed compact object has been theoretically explored3, but signatures for binarity or evidence for the formation of a compact object during a supernova explosion are still lacking. Here we report a stripped-envelope supernova, SN 2022jli, which shows 12.4-day periodic undulations during the declining light curve. Narrow Hα emission is detected in late-time spectra with concordant periodic velocity shifts, probably arising from hydrogen gas stripped from a companion and accreted onto the compact remnant. A new Fermi-LAT γ-ray source is temporally and positionally consistent with SN 2022jli. The observed properties of SN 2022jli, including periodic undulations in the optical light curve, coherent Hα emission shifting and evidence for association with a γ-ray source, point to the explosion of a massive star in a binary system leaving behind a bound compact remnant. Mass accretion from the companion star onto the compact object powers the light curve of the supernova and generates the γ-ray emission.
\n
\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
Using the Zwicky Transient Facility, in 2021 February we identified the first known outburst of the black hole X-ray transient XTE J1859+226 since its discovery in 1999. The outburst was visible at X-ray, UV, and optical wavelengths for less than 20 days, substantially shorter than its full outburst of 320 days in 1999, and the observed peak luminosity was 2 orders of magnitude lower. Its peak bolometric luminosity was only 2 × 1035 erg s−1, implying an Eddington fraction of about 3 × 10−4. The source remained in the hard spectral state throughout the outburst. From optical spectroscopy measurements we estimate an outer disk radius of 1011 cm. The low observed X-ray luminosity is not sufficient to irradiate the entire disk, but we observe a surprising exponential decline in the X-ray light curve. These observations highlight the potential of optical and infrared synoptic surveys to discover low-luminosity activity from X-ray transients.
",
"doi": "10.3847/1538-4357/acf37c",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-10-10",
"series_number": "1",
"volume": "956",
"issue": "1",
"pages": "21"
},
{
"id": "authors:p4rnh-xvp61",
"collection": "authors",
"collection_id": "p4rnh-xvp61",
"cite_using_url": "https://authors.library.caltech.edu/records/p4rnh-xvp61",
"type": "article",
"title": "SN 2020udy: an SN Iax with strict limits on interaction consistent with a helium-star companion",
"author": [
{
"family_name": "Maguire",
"given_name": "Kate",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Magee",
"given_name": "Mark R",
"orcid": "0000-0002-0629-8931"
},
{
"family_name": "Leloudas",
"given_name": "Giorgos",
"orcid": "0000-0002-8597-0756"
},
{
"family_name": "Miller",
"given_name": "Adam A",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Dimitriadis",
"given_name": "Georgios",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Pursiainen",
"given_name": "Miika",
"orcid": "0000-0003-4663-4300"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Perley",
"given_name": "Daniel A",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj R",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Nordin",
"given_name": "Jakob"
},
{
"family_name": "Reusch",
"given_name": "Simeon",
"orcid": "0000-0002-7788-628X"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Terreran",
"given_name": "Giacomo",
"orcid": "0000-0003-0794-5982"
},
{
"family_name": "Yang(\u6768\u8f76)",
"given_name": "Yi",
"orcid": "0000-0002-6535-8500"
},
{
"family_name": "Bellm",
"given_name": "Eric C",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Groom",
"given_name": "Steven L",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Lacroix",
"given_name": "Leander",
"orcid": "0000-0003-0629-5746"
},
{
"family_name": "Masci",
"given_name": "Frank J",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Purdum",
"given_name": "Josiah N",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
}
],
"abstract": "Early observations of transient explosions can provide vital clues to their progenitor origins. In this paper, we present the nearby Type Iax (02cx-like) supernova (SN), SN 2020udy, that was discovered within hours (∼7 h) of estimated first light. An extensive data set of ultra-violet, optical, and near-infrared observations was obtained, covering out to ∼150 d after explosion. SN 2020udy peaked at −17.86 ± 0.43 mag in the r band and evolved similarly to other ‘luminous’ SNe Iax, such as SNe 2005hk and 2012Z. Its well-sampled early light curve allows strict limits on companion interaction to be placed. Main-sequence companion stars with masses of 2 and 6 M\u2299 are ruled out at all viewing angles, while a helium-star companion is allowed from a narrow range of angles (140–180° away from the companion). The spectra and light curves of SN 2020udy are in good agreement with those of the ‘N5def’ deflagration model of a near Chandrasekhar-mass carbon–oxygen white dwarf. However, as has been seen in previous studies of similar luminosity events, SN 2020udy evolves slower than the model. Broad-band linear polarization measurements taken at and after peak are consistent with no polarization, in agreement with the predictions of the companion-star configuration from the early light-curve measurements. The host galaxy environment is low metallicity and is consistent with a young stellar population. Overall, we find the most plausible explosion scenario to be the incomplete disruption of a CO white dwarf near the Chandrasekhar-mass limit, with a helium-star companion.
",
"doi": "10.1093/mnras/stad2316",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2023-10",
"series_number": "1",
"volume": "525",
"issue": "1",
"pages": "1210-1228"
},
{
"id": "authors:5991k-6w460",
"collection": "authors",
"collection_id": "5991k-6w460",
"cite_using_url": "https://authors.library.caltech.edu/records/5991k-6w460",
"type": "article",
"title": "The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves. I. Signatures of H/He-free interaction in the first four months",
"author": [
{
"family_name": "Kuncarayakti",
"given_name": "H.",
"orcid": "0000-0002-1132-1366",
"clpid": "Kuncarayakti-Hanindyo"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Izzo",
"given_name": "L.",
"orcid": "0000-0001-9695-8472"
},
{
"family_name": "Maeda",
"given_name": "K.",
"orcid": "0000-0003-2611-7269"
},
{
"family_name": "Yang",
"given_name": "S."
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Angus",
"given_name": "C. R.",
"orcid": "0000-0002-4269-7999"
},
{
"family_name": "Aubert",
"given_name": "M."
},
{
"family_name": "Auchettl",
"given_name": "K.",
"orcid": "0000-0002-4449-9152"
},
{
"family_name": "Della Valle",
"given_name": "M.",
"orcid": "0000-0003-3142-5020"
},
{
"family_name": "Dessart",
"given_name": "L.",
"orcid": "0000-0003-0599-8407"
},
{
"family_name": "Hinds",
"given_name": "K.",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Kankare",
"given_name": "E.",
"orcid": "0000-0001-8257-3512"
},
{
"family_name": "Kawabata",
"given_name": "M."
},
{
"family_name": "Lundqvist",
"given_name": "P."
},
{
"family_name": "Nakaoka",
"given_name": "T."
},
{
"family_name": "Perley",
"given_name": "D.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Raimundo",
"given_name": "S. I.",
"orcid": "0000-0002-6248-398X"
},
{
"family_name": "Strotjohann",
"given_name": "N. L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Taguchi",
"given_name": "K."
},
{
"family_name": "Cai",
"given_name": "Y.-Z."
},
{
"family_name": "Charalampopoulos",
"given_name": "P."
},
{
"family_name": "Fang",
"given_name": "Q."
},
{
"family_name": "Fraser",
"given_name": "M."
},
{
"family_name": "Guti\u00e9rrez",
"given_name": "C. P."
},
{
"family_name": "Imazawa",
"given_name": "R."
},
{
"family_name": "Kangas",
"given_name": "T."
},
{
"family_name": "Kawabata",
"given_name": "K. S."
},
{
"family_name": "Kotak",
"given_name": "R."
},
{
"family_name": "Kravtsov",
"given_name": "T."
},
{
"family_name": "Matilainen",
"given_name": "K."
},
{
"family_name": "Mattila",
"given_name": "S."
},
{
"family_name": "Moran",
"given_name": "S."
},
{
"family_name": "Murata",
"given_name": "I."
},
{
"family_name": "Salmaso",
"given_name": "I."
},
{
"family_name": "Anderson",
"given_name": "J. P."
},
{
"family_name": "Ashall",
"given_name": "C."
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Benetti",
"given_name": "S."
},
{
"family_name": "Chambers",
"given_name": "K. C."
},
{
"family_name": "Chen",
"given_name": "T.-W."
},
{
"family_name": "Coughlin",
"given_name": "M."
},
{
"family_name": "De Colle",
"given_name": "F."
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Galbany",
"given_name": "L."
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Gromadzki",
"given_name": "M."
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Hajela",
"given_name": "A."
},
{
"family_name": "Inserra",
"given_name": "C."
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Mahabal",
"given_name": "A. A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Martin-Carrillo",
"given_name": "A."
},
{
"family_name": "Moore",
"given_name": "T."
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "T. E."
},
{
"family_name": "Nicholl",
"given_name": "M."
},
{
"family_name": "Ragosta",
"given_name": "F."
},
{
"family_name": "Riddle",
"given_name": "R. L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Srivastav",
"given_name": "S."
},
{
"family_name": "Stritzinger",
"given_name": "M. D."
},
{
"family_name": "Wold",
"given_name": "A.",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery-A"
},
{
"family_name": "Young",
"given_name": "D. R."
}
],
"abstract": "We report on our study of the supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy were used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ~14 000 km s−1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ~ 1000–2500 km s−1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times, such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to blue as the light curve evolves along the second hump, and by the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of mass loss consisting of H/He-free material shortly prior to explosion.
",
"doi": "10.1051/0004-6361/202346526",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2023-10",
"volume": "678",
"pages": "A209"
},
{
"id": "authors:hbgpj-4f191",
"collection": "authors",
"collection_id": "hbgpj-4f191",
"cite_using_url": "https://authors.library.caltech.edu/records/hbgpj-4f191",
"type": "article",
"title": "Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function",
"author": [
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Ravi",
"given_name": "Vikram",
"orcid": "0000-0002-7252-5485",
"clpid": "Ravi-Vikram"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074"
},
{
"family_name": "Lu",
"given_name": "Wenbin",
"orcid": "0000-0002-1568-7461"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"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": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert"
},
{
"family_name": "Ricarte",
"given_name": "Angelo",
"orcid": "0000-0001-5287-0452"
},
{
"family_name": "Chadayammuri",
"given_name": "Urmila"
},
{
"family_name": "Quataert",
"given_name": "Eliot",
"orcid": "0000-0001-9185-5044"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Ben"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We conduct a systematic tidal disruption event (TDE) demographics analysis using the largest sample of optically selected TDEs. A flux-limited, spectroscopically complete sample of 33 TDEs is constructed using the Zwicky Transient Facility over 3 yr (from 2018 October to 2021 September). We infer the black hole (BH) mass (MBH) with host galaxy scaling relations, showing that the sample MBH ranges from 105.1M\u2299 to 108.2M\u2299. We developed a survey efficiency corrected maximum volume method to infer the rates. The rest-frame g-band luminosity function can be well described by a broken power law of \u03d5(Lg)∝[(Lg/Lbk)0.3+(Lg/Lbk)2.6]−1, with Lbk = 1043.1 erg s−1. In the BH mass regime of 105.3 \u2272 (MBH/M\u2299) \u2272 107.3, the TDE mass function follows \u03d5(MBH)∝MBH−0.25, which favors a flat local BH mass function (dnBH/dlogMBH≈constant). We confirm the significant rate suppression at the high-mass end (MBH \u2273 107.5M\u2299), which is consistent with theoretical predictions considering direct capture of hydrogen-burning stars by the event horizon. At a host galaxy mass of Mgal ∼ 1010M\u2299, the average optical TDE rate is ≈3.2 × 10−5 galaxy−1 yr−1. We constrain the optical TDE rate to be [3.7, 7.4, and 1.6] × 10−5 galaxy−1 yr−1 in galaxies with red, green, and blue colors.
",
"doi": "10.3847/2041-8213/acf216",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2023-09-20",
"series_number": "1",
"volume": "955",
"issue": "1",
"pages": "L6"
},
{
"id": "authors:n3y3y-an932",
"collection": "authors",
"collection_id": "n3y3y-an932",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230727-911124400.2",
"type": "article",
"title": "Growth-rate measurement with type-Ia supernovae using ZTF survey simulations",
"author": [
{
"family_name": "Carreres",
"given_name": "Bastien",
"orcid": "0000-0002-7234-844X",
"clpid": "Carreres-Bastien"
},
{
"family_name": "Bautista",
"given_name": "Julian E.",
"orcid": "0000-0002-9885-3989",
"clpid": "Bautista-Julian-E"
},
{
"family_name": "Feinstein",
"given_name": "Fabrice",
"clpid": "Feinstein-Fabrice"
},
{
"family_name": "Fouchez",
"given_name": "Dominique",
"orcid": "0000-0002-7496-3796",
"clpid": "Fouchez-Dominique"
},
{
"family_name": "Racine",
"given_name": "Benjamin",
"orcid": "0000-0001-8861-3052",
"clpid": "Racine-Benjamin"
},
{
"family_name": "Smith",
"given_name": "Mathew",
"orcid": "0000-0002-3321-1432",
"clpid": "Smith-Mathew"
},
{
"family_name": "Amenouche",
"given_name": "Melissa",
"orcid": "0009-0006-7454-3579",
"clpid": "Amenouche-Melissa"
},
{
"family_name": "Aubert",
"given_name": "Marie",
"clpid": "Aubert-Marie"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979",
"clpid": "Dhawan-Suhail"
},
{
"family_name": "Ginolin",
"given_name": "Madeleine",
"clpid": "Ginolin-Madeleine"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996",
"clpid": "Goobar-Ariel"
},
{
"family_name": "Gris",
"given_name": "Philippe",
"orcid": "0000-0001-5673-0959",
"clpid": "Gris-Philippe"
},
{
"family_name": "Lacroix",
"given_name": "Leander",
"clpid": "Lacroix-Leander"
},
{
"family_name": "Nuss",
"given_name": "Eric",
"orcid": "0000-0002-3528-5777",
"clpid": "Nuss-Eric"
},
{
"family_name": "Regnault",
"given_name": "Nicolas",
"orcid": "0000-0001-7029-7901",
"clpid": "Regnault-Nicolas"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560",
"clpid": "Rigault-Mickael"
},
{
"family_name": "Robert",
"given_name": "Estelle",
"orcid": "0000-0002-5339-5996",
"clpid": "Robert-Estelle"
},
{
"family_name": "Rosnet",
"given_name": "Philippe",
"orcid": "0000-0002-6099-7565",
"clpid": "Rosnet-Philippe"
},
{
"family_name": "Sommer",
"given_name": "Kelian",
"orcid": "0009-0007-5504-5838",
"clpid": "Sommer-K\u00e9lian"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Sravan",
"given_name": "Niharika",
"clpid": "Sravan-Niharika"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Purdum",
"given_name": "Josiah N.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
}
],
"abstract": "Measurements of the growth rate of structures at z\u2004< 0.1 using only ZTF SN Ia peculiar velocities. We carefully tested the method and we quantified biases due to selection effects (photometric detection, spectroscopic follow-up for typing) on several independent realizations. We simulated the equivalent of 6 years of ZTF data, and considering an unbiased spectroscopically typed sample at z\u2004f\u03c3\u2088 with an average uncertainty of 19% precision. We also investigated the information gain in applying bias correction methods. Our results validate our framework, which can be used on real ZTF data.",
"doi": "10.1051/0004-6361/202346173",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2023-06",
"volume": "674",
"pages": "Art. No. A197"
},
{
"id": "authors:m3svd-jsx80",
"collection": "authors",
"collection_id": "m3svd-jsx80",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230522-906228000.12",
"type": "article",
"title": "Neutrino follow-up with the Zwicky Transient Facility: results from the first 24 campaigns",
"author": [
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert-D"
},
{
"family_name": "Reusch",
"given_name": "Simeon",
"orcid": "0000-0002-7788-628X",
"clpid": "Reusch-Simeon"
},
{
"family_name": "Franckowiak",
"given_name": "Anna",
"orcid": "0000-0002-5605-2219",
"clpid": "Franckowiak-Anna"
},
{
"family_name": "Kowalski",
"given_name": "Marek",
"orcid": "0000-0001-8594-8666",
"clpid": "Kowalski-Marek"
},
{
"family_name": "Necker",
"given_name": "Jannis",
"orcid": "0000-0003-0280-7484",
"clpid": "Necker-Jannis"
},
{
"family_name": "Weimann",
"given_name": "Sven",
"clpid": "Weimann-Sven"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumada-Tom\u00e1s"
},
{
"family_name": "Amaro\u00a0Seoane",
"given_name": "Pau",
"orcid": "0000-0003-3993-3249",
"clpid": "Amaro-Seoane-Pau"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X",
"clpid": "Bloom-Joshua-S"
},
{
"family_name": "Coughlin",
"given_name": "Michael",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-Michael-W"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154",
"clpid": "Gezari-Suvi"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881",
"clpid": "Kaplan-David-L"
},
{
"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",
"clpid": "Kong-Albert-K-H"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Lincetto",
"given_name": "Massimiliano",
"orcid": "0000-0002-1460-3369",
"clpid": "Lincetto-Massimiliano"
},
{
"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": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659",
"clpid": "Medford-Michael-S"
},
{
"family_name": "Morgan",
"given_name": "Robert",
"orcid": "0000-0002-7016-5471",
"clpid": "Morgan-Robert"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274",
"clpid": "Nordin-Jakob"
},
{
"family_name": "Rodriguez",
"given_name": "Hector",
"clpid": "Rodriguez-Hector"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "van\u00a0Santen",
"given_name": "Jakob",
"orcid": "0000-0002-2412-9728",
"clpid": "van-Santen-Jakob"
},
{
"family_name": "van\u00a0Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-Sjoert"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "The Zwicky Transient Facility (ZTF) performs a systematic neutrino follow-up programme, searching for optical counterparts to high-energy neutrinos with dedicated Target-of-Opportunity (ToO) observations. Since first light in March 2018, ZTF has taken prompt observations for 24 high-quality neutrino alerts from the IceCube Neutrino Observatory, with a median latency of 12.2\u2009h from initial neutrino detection. From two of these campaigns, we have already reported tidal disruption event (TDE) AT 2019dsg and likely TDE AT 2019fdr as probable counterparts, suggesting that TDEs contribute >7.8 per\u2009cent of the astrophysical neutrino flux. We here present the full results of our programme through to December 2021. No additional candidate neutrino sources were identified by our programme, allowing us to place the first constraints on the underlying optical luminosity function of astrophysical neutrino sources. Transients with optical absolutes magnitudes brighter that \u221221 can contribute no more than 87 per\u2009cent of the total, while transients brighter than \u221222 can contribute no more than 58 per\u2009cent of the total, neglecting the effect of extinction and assuming they follow the star formation rate. These are the first observational constraints on the neutrino emission of bright populations such as superluminous supernovae. None of the neutrinos were coincident with bright optical AGN flares comparable to that observed for TXS 0506+056/IC170922A, with such optical blazar flares producing no more than 26 per\u2009cent of the total neutrino flux. We highlight the outlook for electromagnetic neutrino follow-up programmes, including the expected potential for the Rubin Observatory.",
"doi": "10.1093/mnras/stad767",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2023-06",
"series_number": "4",
"volume": "521",
"issue": "4",
"pages": "5046-5063"
},
{
"id": "authors:bppgr-qfb44",
"collection": "authors",
"collection_id": "bppgr-qfb44",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230725-857338000.64",
"type": "article",
"title": "A radio-detected type Ia supernova with helium-rich circumstellar material",
"author": [
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Johansson",
"given_name": "Joel",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Mold\u00f3n",
"given_name": "Javier",
"orcid": "0000-0002-8079-7608"
},
{
"family_name": "Moriya",
"given_name": "Takashi J.",
"orcid": "0000-0003-1169-1954"
},
{
"family_name": "Mattila",
"given_name": "Seppo",
"orcid": "0000-0001-7497-2994"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Chomiuk",
"given_name": "Laura",
"orcid": "0000-0002-8400-3705"
},
{
"family_name": "P\u00e9rez-Torres",
"given_name": "Miguel",
"orcid": "0000-0001-5654-0266"
},
{
"family_name": "Harris",
"given_name": "Chelsea",
"orcid": "0000-0002-1751-7474"
},
{
"family_name": "Lundqvist",
"given_name": "Peter",
"orcid": "0000-0002-3664-8082"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Yang",
"given_name": "Sheng",
"orcid": "0000-0002-2898-6532"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Strotjohann",
"given_name": "Nora Linn",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Lezmy",
"given_name": "Jeremy"
},
{
"family_name": "Maguire",
"given_name": "Kate",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Omand",
"given_name": "Conor",
"orcid": "0000-0002-9646-8710"
},
{
"family_name": "Smith",
"given_name": "Mathew",
"orcid": "0000-0002-3321-1432"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659"
},
{
"family_name": "Park",
"given_name": "Sungmin"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Reynolds",
"given_name": "Thomas M."
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Robert",
"given_name": "Estelle",
"orcid": "0000-0002-5339-5996"
},
{
"family_name": "Ryder",
"given_name": "Stuart D.",
"orcid": "0000-0003-4501-8100"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-Daniel"
}
],
"abstract": "Type Ia supernovae (SNe Ia) are thermonuclear explosions of degenerate white dwarf stars destabilized by mass accretion from a companion star, but the nature of their progenitors remains poorly understood. A way to discriminate between progenitor systems is through radio observations; a non-degenerate companion star is expected to lose material through winds or binary interaction before explosion, and the supernova ejecta crashing into this nearby circumstellar material should result in radio synchrotron emission. However, despite extensive efforts, no type Ia supernova (SN Ia) has ever been detected at radio wavelengths, which suggests a clean environment and a companion star that is itself a degenerate white dwarf star. Here we report on the study of SN 2020eyj, a SN Ia showing helium-rich circumstellar material, as demonstrated by its spectral features, infrared emission and, for the first time in a SN Ia to our knowledge, a radio counterpart. On the basis of our modelling, we conclude that the circumstellar material probably originates from a single-degenerate binary system in which a white dwarf accretes material from a helium donor star, an often proposed formation channel for SNe Ia (refs.\u20096,7). We describe how comprehensive radio follow-up of SN 2020eyj-like SNe Ia can improve the constraints on their progenitor systems.",
"doi": "10.1038/s41586-023-05916-w",
"pmcid": "PMC10191849",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2023-05-18",
"series_number": "7961",
"volume": "617",
"issue": "7961",
"pages": "477-482"
},
{
"id": "authors:xmqkt-16q50",
"collection": "authors",
"collection_id": "xmqkt-16q50",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230613-730222500.6",
"type": "article",
"title": "A Systematic Study of Ia-CSM Supernovae from the ZTF Bright Transient Survey",
"author": [
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Strotjohann",
"given_name": "Nora Linn",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Maguire",
"given_name": "Kate",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Bruch",
"given_name": "Rachel",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "Deckers",
"given_name": "Maxime",
"orcid": "0000-0001-8857-9843"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"orcid": "0000-0001-7344-0208"
},
{
"family_name": "Filippenko",
"given_name": "Alexei V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Goldwasser",
"given_name": "Samantha"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Hankins",
"given_name": "Matt",
"orcid": "0000-0001-9315-8437"
},
{
"family_name": "Jencson",
"given_name": "Jacob",
"orcid": "0000-0001-5754-4007"
},
{
"family_name": "Johansson",
"given_name": "Joel P.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"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": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Nir",
"given_name": "Guy",
"orcid": "0000-0002-7501-5579"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Schweyer",
"given_name": "Tassilo",
"orcid": "0000-0001-8948-3456"
},
{
"family_name": "Terwel",
"given_name": "Jacco H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yang",
"given_name": "Yi",
"orcid": "0000-0002-6535-8500"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
}
],
"abstract": "Among the supernovae (SNe) that show strong interaction with a circumstellar medium (CSM), there is a rare subclass of Type Ia supernovae, SNe Ia-CSM, which show strong narrow hydrogen emission lines much like SNe IIn but on top of a diluted Type Ia spectrum. The only previous systematic study of this class identified 16 SNe Ia-CSM, eight historic and eight from the Palomar Transient Factory (PTF). Now using the successor survey to PTF, the Zwicky Transient Facility (ZTF), we have classified 12 additional SNe Ia-CSM through the systematic Bright Transient Survey (BTS). Consistent with previous studies, we find these SNe to have slowly evolving optical light curves with peak absolute magnitudes between \u221219.1 and \u221221, spectra having weak H\u03b2 and large Balmer decrements of \u223c7. Out of the 10 SNe from our sample observed by NEOWISE, nine have 3\u03c3 detections, with some SNe showing a reduction in the red wing of H\u03b1, indicative of newly formed dust. We do not find our SN Ia-CSM sample to have a significantly different distribution of equivalent widths of He I\u03bb5876 than SNe IIn as observed in Silverman et al. The hosts tend to be late-type galaxies with recent star formation. We derive a rate estimate of 29\u207a\u00b2\u2077\u208b\u2082\u2081Gpc\u207b\u00b3 yr\u207b\u00b9 for SNe Ia-CSM, which is \u223c0.02%\u20130.2% of the SN Ia rate. We also identify six ambiguous SNe IIn/Ia-CSM in the BTS sample and including them gives an upper limit rate of 0.07%\u20130.8%. This work nearly doubles the sample of well-studied Ia-CSM objects in Silverman et al., increasing the total number to 28.",
"doi": "10.3847/1538-4357/acbc16",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-05-01",
"series_number": "1",
"volume": "948",
"issue": "1",
"pages": "Art. No. 52"
},
{
"id": "authors:0rrwq-ekb08",
"collection": "authors",
"collection_id": "0rrwq-ekb08",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230613-731854300.61",
"type": "article",
"title": "SN\u20092021zny: an early flux excess combined with late-time oxygen emission suggests a double white dwarf merger event",
"author": [
{
"family_name": "Dimitriadis",
"given_name": "Georgios",
"orcid": "0000-0001-9494-179X",
"clpid": "Dimitriadis-Georgios"
},
{
"family_name": "Maguire",
"given_name": "Kate",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj R.",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Lebron",
"given_name": "Ryan J."
},
{
"family_name": "Liu",
"given_name": "Chang",
"orcid": "0000-0002-7866-4531"
},
{
"family_name": "Kozyreva",
"given_name": "Alexandra",
"orcid": "0000-0001-9598-8821"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Ridden-Harper",
"given_name": "Ryan",
"orcid": "0000-0003-1724-2885"
},
{
"family_name": "Anderson",
"given_name": "Joseph P.",
"orcid": "0000-0003-0227-3451"
},
{
"family_name": "Chen",
"given_name": "Ting-Wan",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Coughlin",
"given_name": "Michael",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Valle",
"given_name": "Massimo Della",
"orcid": "0000-0003-3142-5020"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Galbany",
"given_name": "Llu\u00eds",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Gromadzki",
"given_name": "Mariusz",
"orcid": "0000-0002-1650-1518"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Guti\u00e9rrez",
"given_name": "Claudia P.",
"orcid": "0000-0003-2375-2064"
},
{
"family_name": "Ihanec",
"given_name": "Nada"
},
{
"family_name": "Inserra",
"given_name": "Cosimo",
"orcid": "0000-0002-3968-4409"
},
{
"family_name": "Johansson",
"given_name": "Joel",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "Tom\u00e1s E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Polin",
"given_name": "Abigail",
"orcid": "0000-0002-1633-6495",
"clpid": "Polin-Abigail"
},
{
"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": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Srivastav",
"given_name": "Shubham",
"orcid": "0000-0003-4524-6883"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Wang",
"given_name": "Qinan",
"orcid": "0000-0001-5233-6989"
},
{
"family_name": "Yang",
"given_name": "Yi",
"orcid": "0000-0002-9024-4150"
},
{
"family_name": "Young",
"given_name": "David R.",
"orcid": "0000-0002-1229-2499"
}
],
"abstract": "We present a photometric and spectroscopic analysis of the ultraluminous and slowly evolving 03fg-like Type Ia SN\u20092021zny. Our observational campaign starts from \u223c5.3 h after explosion (making SN\u20092021zny one of the earliest observed members of its class), with dense multiwavelength coverage from a variety of ground- and space-based telescopes, and is concluded with a nebular spectrum \u223c10 months after peak brightness. SN\u20092021zny displayed several characteristics of its class, such as the peak brightness (M_B = \u221219.95 mag), the slow decline (\u0394m_(15)(B) = 0.62 mag), the blue early-time colours, the low ejecta velocities, and the presence of significant unburned material above the photosphere. However, a flux excess for the first \u223c1.5 d after explosion is observed in four photometric bands, making SN\u20092021zny the third 03fg-like event with this distinct behaviour, while its +313 d spectrum shows prominent [O \u026a] lines, a very unusual characteristic of thermonuclear SNe. The early flux excess can be explained as the outcome of the interaction of the ejecta with \u223c0.04M_\u2299 of H/He-poor circumstellar material at a distance of \u223c10^(12) cm, while the low ionization state of the late-time spectrum reveals low abundances of stable iron-peak elements. All our observations are in accordance with a progenitor system of two carbon/oxygen white dwarfs that undergo a merger event, with the disrupted white dwarf ejecting carbon-rich circumstellar material prior to the primary white dwarf detonation.",
"doi": "10.1093/mnras/stad536",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2023-05",
"series_number": "1",
"volume": "521",
"issue": "1",
"pages": "1162-1183"
},
{
"id": "authors:8pb0w-gz790",
"collection": "authors",
"collection_id": "8pb0w-gz790",
"cite_using_url": "https://authors.library.caltech.edu/records/8pb0w-gz790",
"type": "article",
"title": "SN 2020jgb: A Peculiar Type Ia Supernova Triggered by a Helium-shell Detonation in a Star-forming Galaxy",
"author": [
{
"family_name": "Liu \u5218",
"given_name": "Chang \u7545",
"orcid": "0000-0002-7866-4531"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Polin",
"given_name": "Abigail",
"orcid": "0000-0002-1633-6495",
"clpid": "Polin-Abigail"
},
{
"family_name": "Nugent",
"given_name": "Anya E.",
"orcid": "0000-0002-2028-9329"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Nugent",
"given_name": "Peter E.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Blanchard",
"given_name": "Peter",
"orcid": "0000-0003-0526-2248"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Filippenko",
"given_name": "Alexei V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Maguire",
"given_name": "Kate",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Schweyer",
"given_name": "Tassilo",
"orcid": "0000-0001-8948-3456"
},
{
"family_name": "Sears",
"given_name": "Huei",
"orcid": "0000-0001-8023-4912"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-David"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Racine",
"given_name": "Benjamin",
"orcid": "0000-0001-8861-3052"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "\n
The detonation of a thin (\u22720.03 M\u2299) helium shell (He-shell) atop a ∼1 M\u2299 white dwarf (WD) is a promising mechanism to explain normal Type Ia supernovae (SNe Ia), while thicker He-shells and less massive WDs may explain some recently observed peculiar SNe Ia. We present observations of SN 2020jgb, a peculiar SN Ia discovered by the Zwicky Transient Facility (ZTF). Near maximum brightness, SN 2020jgb is slightly subluminous (ZTF g-band absolute magnitude −18.7 mag \u2272 Mg \u2272 −18.2 mag depending on the amount of host-galaxy extinction) and shows an unusually red color (0.2 mag \u2272 gZTF − rZTF \u2272 0.4 mag) due to strong line-blanketing blueward of ∼5000 Å. These properties resemble those of SN 2018byg, a peculiar SN Ia consistent with an He-shell double detonation (DDet) SN. Using detailed radiative transfer models, we show that the optical spectroscopic and photometric evolution of SN 2020jgb is broadly consistent with a ∼0.95–1.00 M\u2299 (C/O core + He-shell) progenitor ignited by a \u22730.1 M\u2299 He-shell. However, one-dimensional radiative transfer models without non-local-thermodynamic-equilibrium treatment cannot accurately characterize the line-blanketing features, making the actual shell mass uncertain. We detect a prominent absorption feature at ∼1 μm in the near-infrared (NIR) spectrum of SN 2020jgb, which might originate from unburnt helium in the outermost ejecta. While the sample size is limited, we find similar 1 μm features in all the peculiar He-shell DDet candidates with NIR spectra obtained to date. SN 2020jgb is also the first peculiar He-shell DDet SN discovered in a star-forming dwarf galaxy, indisputably showing that He-shell DDet SNe occur in both star-forming and passive galaxies, consistent with the normal SN Ia population.
\n
We present a sample of 14 hydrogen-rich superluminous supernovae (SLSNe II) from the Zwicky Transient Facility (ZTF) between 2018 and 2020. We include all classified SLSNe with peaks M_g < −20 mag with observed broad but not narrow Balmer emission, corresponding to roughly 20 per cent of all hydrogen-rich SLSNe in ZTF phase I. We examine the light curves and spectra of SLSNe II and attempt to constrain their power source using light-curve models. The brightest events are photometrically and spectroscopically similar to the prototypical SN 2008es, while others are found spectroscopically more reminiscent of non-superluminous SNe II, especially SNe II-L. \u2075\u2076Ni decay as the primary power source is ruled out. Light-curve models generally cannot distinguish between circumstellar interaction (CSI) and a magnetar central engine, but an excess of ultraviolet (UV) emission signifying CSI is seen in most of the SNe with UV data, at a wide range of photometric properties. Simultaneously, the broad H α profiles of the brightest SLSNe II can be explained through electron scattering in a symmetric circumstellar medium (CSM). In other SLSNe II without narrow lines, the CSM may be confined and wholly overrun by the ejecta. CSI, possibly involving mass lost in recent eruptions, is implied to be the dominant power source in most SLSNe II, and the diversity in properties is likely the result of different mass loss histories. Based on their radiated energy, an additional power source may be required for the brightest SLSNe II, however – possibly a central engine combined with CSI.
",
"doi": "10.1093/mnras/stac2218",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2022-10",
"series_number": "1",
"volume": "516",
"issue": "1",
"pages": "1193-1218"
},
{
"id": "authors:6jqva-j0p89",
"collection": "authors",
"collection_id": "6jqva-j0p89",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220825-833128900.760",
"type": "article",
"title": "Discovery of the First Known Asteroid Confined within the Orbit of Venus",
"author": [
{
"family_name": "Ip",
"given_name": "Wing-Huen",
"orcid": "0000-0002-3140-5014",
"clpid": "Ip-Wing-Huen"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Ye",
"given_name": "Quanzhi",
"orcid": "0000-0002-4838-7676",
"clpid": "Ye-Quanzhi"
},
{
"family_name": "Kramer",
"given_name": "Emily A.",
"orcid": "0000-0003-0457-2519",
"clpid": "Kramer-Emily-A"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-A-J"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
}
],
"abstract": "We report on the discovery by the Zwicky Transient Facility of an asteroid orbiting entirely within the orbit of Venus, the first known example of this orbital class. The asteroid's perihelion is closer to the Sun than the aphelion of Mercury, and its diameter is estimated at about 1.8 km assuming an albedo of 0.2. The object was first observed on 2020 January 4 in four exposures obtained 7 minutes apart during an evening twilight survey. Its IAU-recognized designation is 594913 'Ayl\u00f3'chaxnim.",
"doi": "10.3847/2041-8213/ac8470",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2022-08-10",
"series_number": "1",
"volume": "935",
"issue": "1",
"pages": "Art. No. L6"
},
{
"id": "authors:aaqg0-dmd73",
"collection": "authors",
"collection_id": "aaqg0-dmd73",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220525-93069000",
"type": "article",
"title": "Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period\u2013Luminosity\u2013Metallicity and Period\u2013Wesenheit\u2013Metallicity Relations",
"author": [
{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554",
"clpid": "Ngeow-Chow-Choong"
},
{
"family_name": "Bhardwaj",
"given_name": "Anupam",
"orcid": "0000-0001-6147-3360",
"clpid": "Bhardwaj-A"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"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": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659",
"clpid": "Medford-Michael-S"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
}
],
"abstract": "Based on time-series observations collected from the Zwicky Transient Facility (ZTF), we derived period\u2013luminosity\u2013metallicity (PLZ) and period\u2013Wesenheit\u2013metallicity (PWZ) relations for RR Lyrae located in globular clusters. We have applied various selection criteria to exclude RR Lyrae with problematic or spurious light curves. These selection criteria utilized information on the number of data points per light curve, amplitudes, colors, and residuals on the period\u2013luminosity and/or period\u2013Wesenheit relations. Due to blending, a number of RR Lyrae in globular clusters were found to be anomalously bright and have small amplitudes of their ZTF light curves. We used our final sample of \u223c750 RR Lyrae in 46 globular clusters covering a wide metallicity range (\u22122.36 dex < [Fe/H] gri bands. In addition, we have also derived the period\u2013color\u2013metallicity and, for the first time, the period-Q-index-metallicity relations, where the Q-index is extinction-free by construction. We have compared our various relations to empirical and theoretical relations available in the literature and found a good agreement with most studies. Finally, we applied our derived PLZ relation to a dwarf galaxy, Crater II, and found that its true distance modulus should be larger than the most recent determination.",
"doi": "10.3847/1538-3881/ac617e",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-05",
"series_number": "5",
"volume": "163",
"issue": "5",
"pages": "Art. No. 239"
},
{
"id": "authors:qgqdz-p2n39",
"collection": "authors",
"collection_id": "qgqdz-p2n39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220526-173305519",
"type": "monograph",
"title": "Neutrino follow-up with the Zwicky Transient Facility: Results from the first 24 campaigns",
"author": [
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert-D"
},
{
"family_name": "Reusch",
"given_name": "Simeon",
"orcid": "0000-0002-7788-628X"
},
{
"family_name": "Franckowiak",
"given_name": "Anna",
"orcid": "0000-0002-5605-2219"
},
{
"family_name": "Kowalski",
"given_name": "Marek",
"orcid": "0000-0001-8594-8666"
},
{
"family_name": "Necker",
"given_name": "Jannis",
"orcid": "0000-0003-0280-7484"
},
{
"family_name": "Weimann",
"given_name": "Sven"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430"
},
{
"family_name": "Amaro Seoane",
"given_name": "Pau",
"orcid": "0000-0003-3993-3249"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya-G"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Coughlin",
"given_name": "Michael",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"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": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Lincetto",
"given_name": "Massimiliano",
"orcid": "0000-0002-1460-3369"
},
{
"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": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659"
},
{
"family_name": "Morgan",
"given_name": "Robert",
"orcid": "0000-0002-7016-5471"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Rodriguez",
"given_name": "Hector",
"clpid": "Rodriguez-Hector"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "van Santen",
"given_name": "Jakob",
"orcid": "0000-0002-2412-9728"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "The Zwicky Transient Transient Facility (ZTF) performs a systematic neutrino follow-up program, searching for optical counterparts to high-energy neutrinos with dedicated Target-of-Opportunity (ToO) observations. Since first light in March 2018, ZTF has taken prompt observations for 24 high-quality neutrino alerts from the IceCube Neutrino Observatory, with a median latency of 12.2 hours from initial neutrino detection. From two of these campaigns, we have already reported tidal disruption event (TDE) AT2019dsg and likely TDE AT2019fdr as probable counterparts, suggesting that TDEs contribute >7.8% of the astrophysical neutrino flux. We here present the full results of our program through to December 2021. No additional candidate neutrino sources were identified by our program, allowing us to place the first constraints on the underlying optical luminosity function of astrophysical neutrino sources. Transients with optical absolutes magnitudes brighter that -21 can contribute no more than 87% of the total, while transients brighter than -22 can contribute no more than 58% of the total, neglecting the effect of extinction. These are the the first observational constraints on the neutrino emission of bright populations such as superluminous supernovae. None of the neutrinos were coincident with bright optical AGN flares comparable to that observed for TXS 0506+056/IC170922A, suggesting that most astrophysical neutrinos are not produced during such optical flares. We highlight the outlook for electromagnetic neutrino follow-up programs, including the expected potential for the Rubin Observatory.",
"doi": "10.48550/arXiv.2203.17135",
"publisher": "arXiv",
"publication_date": "2022-03-31"
},
{
"id": "authors:wks9q-eg059",
"collection": "authors",
"collection_id": "wks9q-eg059",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220526-173258641",
"type": "monograph",
"title": "The Final Season Reimagined: 30 Tidal Disruption Events from the ZTF-I Survey",
"author": [
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703",
"clpid": "Hammerstein-Erica"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-Sjoert"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154",
"clpid": "Gezari-Suvi"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-Bradley"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"orcid": "0000-0002-4557-6682",
"clpid": "Ward-Charlotte-A"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X",
"clpid": "Frederick-Sara"
},
{
"family_name": "Villanueva",
"given_name": "Natalia",
"clpid": "Villanueva-Natalia"
},
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-Daniel"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659",
"clpid": "Medford-Michael-S"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes"
}
],
"abstract": "Tidal disruption events (TDEs) offer a unique way to study dormant black holes. While the number of observed TDEs has grown thanks to the emergence of wide-field surveys in the past few decades, questions regarding the nature of the observed optical, UV, and X-ray emission remain. We present a uniformly selected sample of 30 spectroscopically classified TDEs from the Zwicky Transient Facility Phase I survey operations with follow-up Swift UV and X-ray observations. Through our investigation into correlations between light curve properties, we recover a shallow positive correlation between the peak bolometric luminosity and decay timescales. We introduce a new spectroscopic class of TDE, TDE-featureless, which are characterized by featureless optical spectra. We recover a difference between the light curve timescales of the four TDE classes, with TDE-H+He having longer rise times. The new TDE-featureless class shows larger peak bolometric luminosities, peak blackbody temperatures, and peak blackbody radii. We examine the differences between the X-ray bright and X-ray faint populations of TDEs in this sample, finding that X-ray bright TDEs show longer decay timescales than the X-ray faint sub-sample. We present a scheme for classifying the shapes of the optical light curves, finding that TDEs with \"structured\" light curves have significantly less massive host galaxies than other types of TDEs. This sample of optically selected TDEs is the largest sample of TDEs from a single survey yet, and the systematic discovery, classification, and follow-up of this sample allows for robust characterization of TDE properties, an important stepping stone looking forward toward the Rubin era.",
"doi": "10.48550/arXiv.2203.01461",
"publisher": "arXiv",
"publication_date": "2022-03-03"
},
{
"id": "authors:wts64-v4b26",
"collection": "authors",
"collection_id": "wts64-v4b26",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220118-993586000",
"type": "article",
"title": "Impact of the SpaceX Starlink Satellites on the Zwicky Transient Facility Survey Observations",
"author": [
{
"family_name": "Mr\u00f3z",
"given_name": "Przemek",
"orcid": "0000-0001-7016-1692",
"clpid": "Mr\u00f3z-Przemek"
},
{
"family_name": "Otarola",
"given_name": "Angel",
"orcid": "0000-0002-9789-2564",
"clpid": "Otarola-Angel"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Medford",
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"abstract": "There is a growing concern about an impact of low-Earth-orbit (LEO) satellite constellations on ground-based astronomical observations, in particular, on wide-field surveys in the optical and infrared. The Zwicky Transient Facility (ZTF), thanks to the large field of view of its camera, provides an ideal setup to study the effects of LEO megaconstellations\u2014such as SpaceX's Starlink\u2014on astronomical surveys. Here, we analyze the archival ZTF observations collected between 2019 November and 2021 September and find 5301 satellite streaks that can be attributed to Starlink satellites. We find that the number of affected images is increasing with time as SpaceX deploys more satellites. Twilight observations are particularly affected\u2014a fraction of streaked images taken during twilight has increased from less than 0.5% in late 2019 to 18% in 2021 August. We estimate that once the size of the Starlink constellation reaches 10,000, essentially all ZTF images taken during twilight may be affected. However, despite the increase in satellite streaks observed during the analyzed period, the current science operations of ZTF are not yet strongly affected. We also find that redesigning Starlink satellites (by installing visors intended to block sunlight from reaching the satellite antennas to prevent reflection) reduces their brightness by a factor of 4.6 \u00b1 0.1 with respect to the original design in g, r, and i bands.",
"doi": "10.3847/2041-8213/ac470a",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2022-01-10",
"series_number": "2",
"volume": "924",
"issue": "2",
"pages": "Art. No. L30"
},
{
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"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190213-135514906",
"type": "article",
"title": "The Zwicky Transient Facility: Science Objectives",
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],
"abstract": "The Zwicky Transient Facility (ZTF), a public\u2013private enterprise, is a new time-domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg^2 field of view and an 8 second readout time. It is well positioned in the development of time-domain astronomy, offering operations at 10% of the scale and style of the Large Synoptic Survey Telescope (LSST) with a single 1-m class survey telescope. The public surveys will cover the observable northern sky every three nights in g and r filters and the visible Galactic plane every night in g and r. Alerts generated by these surveys are sent in real time to brokers. A consortium of universities that provided funding (\"partnership\") are undertaking several boutique surveys. The combination of these surveys producing one million alerts per night allows for exploration of transient and variable astrophysical phenomena brighter than r ~ 20.5 on timescales of minutes to years. We describe the primary science objectives driving ZTF, including the physics of supernovae and relativistic explosions, multi-messenger astrophysics, supernova cosmology, active galactic nuclei, and tidal disruption events, stellar variability, and solar system objects.",
"doi": "10.1088/1538-3873/ab006c",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-07",
"series_number": "1001",
"volume": "131",
"issue": "1001",
"pages": "Art. No. 078001"
},
{
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"collection_id": "k5v2n-n5r58",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190329-083647975",
"type": "article",
"title": "Multiple Outbursts of Asteroid (6478) Gault",
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"clpid": "Prince-T-A"
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"abstract": "Main-belt asteroid (6478) Gault unexpectedly sprouted two tails in late 2018 and early 2019, identifying it as a new active asteroid. Here we present observations obtained by the 1.2 m Zwicky Transient Facility survey telescope that provide detailed time-series coverage of the onset and evolution of Gault's activity. Gault exhibited two brightening events, with the first one starting on 2018 October 18 \u00b1 5 days and a second one starting on 2018 December 24 \u00b1 1 days. The amounts of mass released are 2 \u00d7 10^7 kg and 1 \u00d7 10^6 kg, respectively. Based on photometric measurements, each event persisted for about a month. Gault's color has not changed appreciably over time, with a pre-outburst color of g_(PS1) \u2212 r_(PS1) = 0.50 \u00b1 0.04 and g_(PS1) \u2212 r_(PS1) = 0.46 \u00b1 0.04 during the two outbursts. Simulations of dust dynamics shows that the ejecta consists of dust grains of up to 10 \u03bcm in size that are ejected at low velocities below 1 m s^(-1) regardless of particle sizes. This is consistent with non-sublimation-driven ejection events. The size distribution of the dust exhibits a broken power law, with particles at 10\u201320 \u03bcm following a power law of \u22122.5 to \u22123.0, while larger particles follow a steeper slope of \u22124.0. The derived properties can be explained by either rotational excitation of the nucleus or a merger of a near-contact binary, with the latter scenario to be statistically more likely.",
"doi": "10.3847/2041-8213/ab0f3c",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-04-01",
"series_number": "2",
"volume": "874",
"issue": "2",
"pages": "Art. No. L16"
},
{
"id": "authors:f58y4-9tk79",
"collection": "authors",
"collection_id": "f58y4-9tk79",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181207-084047368",
"type": "article",
"title": "The Zwicky Transient Facility: System Overview, Performance, and First Results",
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],
"abstract": "The Zwicky Transient Facility (ZTF) is a new optical time-domain survey that uses the Palomar 48 inch Schmidt telescope. A custom-built wide-field camera provides a 47 deg^2 field of view and 8 s readout time, yielding more than an order of magnitude improvement in survey speed relative to its predecessor survey, the Palomar Transient Factory. We describe the design and implementation of the camera and observing system. The ZTF data system at the Infrared Processing and Analysis Center provides near-real-time reduction to identify moving and varying objects. We outline the analysis pipelines, data products, and associated archive. Finally, we present on-sky performance analysis and first scientific results from commissioning and the early survey. ZTF's public alert stream will serve as a useful precursor for that of the Large Synoptic Survey Telescope.",
"doi": "10.1088/1538-3873/aaecbe",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-01",
"series_number": "995",
"volume": "131",
"issue": "995",
"pages": "Art. No. 018002"
}
]