[ { "id": "authors:1jnvj-gwn20", "collection": "authors", "collection_id": "1jnvj-gwn20", "cite_using_url": "https://authors.library.caltech.edu/records/1jnvj-gwn20", "type": "monograph", "title": "A generative model for Gaia astrometric orbit catalogs: selection functions for binary stars, giant planets, and compact object companions", "author": [ { "family_name": "El-Badry", "given_name": "Kareem", "orcid": "0000-0002-6871-1752", "clpid": "El-Badry-Kareem" }, { "family_name": "Lam", "given_name": "Casey", "clpid": "Lam-Casey" }, { "family_name": "Holl", "given_name": "Berry", "clpid": "Holl-Berry" }, { "family_name": "Halbwachs", "given_name": "Jean-Louis", "clpid": "Halbwachs-Jean-Louis" }, { "family_name": "Rix", "given_name": "Hans-Walter", "clpid": "Rix-Hans-Walter" }, { "family_name": "Mazeh", "given_name": "Tsevi", "clpid": "Mazeh-Tsevi" }, { "family_name": "Shahaf", "given_name": "Sahar", "clpid": "Shahaf-Sahar" } ], "abstract": "

Astrometry from Gaia DR3 has produced a sample of ∼170,000 Keplerian orbital solutions, with many more anticipated in the next few years. These data have enormous potential to constrain the population of binary stars, giant planets, and compact objects in the Solar neighborhood. But in order to use the published orbit catalogs for statistical inference, it is necessary to understand their selection function: what is the probability that a binary with a given set of properties ends up in a catalog? We show that such a selection function for the Gaia DR3 astrometric binary catalog can be forward-modeled from the Gaia scanning law, including individual 1D astrometric measurements, the fitting of a cascade of astrometric models, and quality cuts applied in post-processing. We populate a synthetic Milky Way model with binary stars and generate a mock catalog of astrometric orbits. The mock catalog is quite similar to the DR3 astrometric binary sample, suggesting that our selection function is a sensible approximation of reality. Our fitting also produces a sample of spurious astrometric orbits similar to those found in DR3; these are mainly the result of scan angle-dependent astrometric biases in marginally resolved wide binaries. We show that Gaia's sensitivity to astrometric binaries falls off rapidly at high eccentricities, but only weakly at high inclinations. We predict that DR4 will yield ∼1 million astrometric orbits, mostly for bright (G\u227215) systems with long periods (Porb\u22731000 d). We provide code to simulate and fit realistic Gaia epoch astrometry for any data release and determine whether any hypothetical binary would receive a cataloged orbital solution.

", "doi": "10.48550/arXiv.2411.00088", "issn": "2565-6120", "publisher": "ArXiv", "publication": "The Open Journal of Astrophysics", "publication_date": "2024-10-31", "volume": "7" }, { "id": "authors:mkhnn-26969", "collection": "authors", "collection_id": "mkhnn-26969", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230130-184111054", "type": "monograph", "title": "15000 Ellipsoidal Binary Candidates in TESS: Orbital Periods, Binary Fraction, and Tertiary Companions", "author": [ { "family_name": "Green", "given_name": "Matthew J.", "orcid": "0000-0002-0948-4801", "clpid": "Green-Matthew-J" }, { "family_name": "Maoz", "given_name": "Dan", "orcid": "0000-0002-6579-0483", "clpid": "Maoz-Dan" }, { "family_name": "Mazeh", "given_name": "Tsevi", "orcid": "0000-0002-3569-3391", "clpid": "Mazeh-Tsevi" }, { "family_name": "Faigler", "given_name": "Simchon", "orcid": "0000-0002-8368-5724", "clpid": "Faigler-Simchon" }, { "family_name": "Shahaf", "given_name": "Sahar", "orcid": "0000-0001-9298-8068", "clpid": "Shahaf-Sahar" }, { "family_name": "Gomel", "given_name": "Roy", "orcid": "0000-0003-2602-5225", "clpid": "Gomel-Roy" }, { "family_name": "El-Badry", "given_name": "Kareem", "orcid": "0000-0002-6871-1752", "clpid": "El-Badry-Kareem" }, { "family_name": "Rix", "given_name": "Hans-Walter", "orcid": "0000-0003-4996-9069", "clpid": "Rix-Hans-Walter" } ], "abstract": "We present a homogeneously-selected sample of 15779 candidate binary systems with main sequence primary stars and orbital periods shorter than 5 days. The targets were selected from TESS full-frame image lightcurves on the basis of their tidally-induced ellipsoidal modulation. Spectroscopic follow-up suggests a sample purity of 83 \u00b1 13 per cent. Injection-recovery tests allow us to estimate our overall completeness as 28 \u00b1 3 per cent with P_(orb) < 3 days and to quantify our selection effects. We estimate that 39 \u00b1 4 per cent of our sample are contact binary systems, and we disentangle the period distributions of the contact and detached binaries. We derive the orbital period distribution of the main sequence binary population at short orbital periods, finding a distribution continuous with the log-normal distribution previously found for solar-type stars at longer periods, but with a significant steepening at P_(orb) \u2272 3 days, and a pile-up of contact binaries at P_(orb) \u2248 0.4 days. Companions in the period range 1--5 days are found to be an order of magnitude more frequent around stars hotter than \u22486250K (the Kraft break) when compared to cooler stars, suggesting that magnetic braking plays an important role in shaping the temperature and period distributions. We detect resolved tertiary companions to 9.0 \u00b1 0.2 per cent of our binaries with a median separation of 3200 AU. The frequency of tertiary companions rises to 29 \u00b1 5 per cent among the systems with the shortest ellipsoidal periods. This large binary sample with quantified selection effects will be a powerful resource for future studies of detached and contact binary systems with P_(orb) < 5 days.", "doi": "10.48550/arXiv.2211.06194", "publisher": "arXiv", "publication_date": "2022-11-11" }, { "id": "authors:0nmyn-79e88", "collection": "authors", "collection_id": "0nmyn-79e88", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230130-184114442", "type": "monograph", "title": "The C/N ratio from FUV spectroscopy as a constraint upon the past evolution of HS0218+3229", "author": [ { "family_name": "Toloza", "given_name": "Odette", "orcid": "0000-0002-2398-719X", "clpid": "Toloza-Odette" }, { "family_name": "G\u00e4ensicke", "given_name": "Boris T.", "orcid": "0000-0002-2761-3005", "clpid": "G\u00e4ensicke-Boris-T" }, { "family_name": "Guzm\u00e1n-Rincon", "given_name": "Laura M.", "clpid": "Guzm\u00e1n-Rincon-Laura-M" }, { "family_name": "Marsh", "given_name": "Tom R.", "orcid": "0000-0002-2498-7589", "clpid": "Marsh-Thomas-R" }, { "family_name": "Szkody", "given_name": "Paula", "orcid": "0000-0003-4373-7777", "clpid": "Szkody-Paula" }, { "family_name": "Schreiber", "given_name": "Matthias R.", "orcid": "0000-0003-3903-8009", "clpid": "Schreiber-Matthias-R" }, { "family_name": "de Martino", "given_name": "Domitilla", "orcid": "0000-0002-5069-4202", "clpid": "de-Martino-Domitilla" }, { "family_name": "Zorotovic", "given_name": "Monica", "orcid": "0000-0002-4526-0469", "clpid": "Zorotovic-Monica" }, { "family_name": "El-Badry", "given_name": "Kareem", "orcid": "0000-0002-6871-1752", "clpid": "El-Badry-Kareem" }, { "family_name": "Koester", "given_name": "Detlev", "orcid": "0000-0002-6164-6978", "clpid": "Koester-Detlev" }, { "family_name": "Lagos", "given_name": "Felipe", "clpid": "Lagos-Felipe" } ], "abstract": "Some white dwarfs accreting from non-degenerate companions show anomalous carbon and nitrogen abundances in the photospheres of their stellar components which have been postulated to be descendants of supersoft X-ray binaries. Therefore the carbon-to-nitrogen ratio can provide constraints upon their past evolution. We fit far ultraviolet spectroscopy of the cataclysmic variable HS0218+3229 taken with the Cosmic Origins Spectrograph using Markov Chain Monte Carlo. While some parameters depend upon the amount of reddening, the carbon-to-nitrogen ratio is about one tenth of the Solar value (log C/N = \u22120.53^(+0.13)_(\u22120.14) and \u22120.58^(+0.16)_(\u22120.15) for almost no reddening and E(B-V) = 0.065, respectively, which are consistent within the uncertainties). We also provide estimates of the silicon and aluminum abundances, and upper limits for iron and oxygen. Using the measured parameters of HS0218+3229 we reconstruct its past using evolutionary simulations with MESA. We implemented Gaussian process fits to the MESA grid in order to determiner the most likely initial binary configuration of HS0218+3229. We found that an initial mass of the donor of M_(donor;i) = 0.90\u22120.98, M_\u2299 and an initial orbital period of P_(orb;i) = 2.88 days (P_(orb;i) = 3.12\u22123.16 days) for an assumed white dwarf mass of M_(WD) = 0.83 M_\u2299 (M_(WD) = 0.60 M_\u2299) are needed to replicate the measured parameters. These configurations imply that the system did not go through a phase of quasi-steady hydrogen-burning on the white dwarf's surface. However, it could have experienced a phase of thermal timescale mass transfer in the past if the initial mass ratio was \u22651.5. We predict that HS0218+3229 will evolve into a CV with a period below the \u224380\\,min period minimum for normal CVs, displaying helium and hydrogen in its spectrum.", "doi": "10.48550/arXiv.2209.06873", "publisher": "arXiv", "publication_date": "2022-09-14" }, { "id": "authors:m10th-f8m82", "collection": "authors", "collection_id": "m10th-f8m82", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230130-184121391", "type": "monograph", "title": "Discovery of Two Polars from a Crossmatch of ZTF and the SRG/eFEDS X-ray Catalog", "author": [ { "family_name": "Rodriguez", "given_name": "Antonio C.", "orcid": "0000-0003-4189-9668", "clpid": "Rodriguez-Antonio-C" }, { "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": "Szkody", "given_name": "Paula", "orcid": "0000-0003-4373-7777", "clpid": "Szkody-Paula" }, { "family_name": "Burdge", "given_name": "Kevin B.", "orcid": "0000-0002-7226-836X", "clpid": "Burdge-Kevin-B" }, { "family_name": "Caiazzo", "given_name": "Ilaria", "orcid": "0000-0002-4770-5388", "clpid": "Caiazzo-Ilaria" }, { "family_name": "van Roestel", "given_name": "Jan", "orcid": "0000-0002-2626-2872", "clpid": "van-Roestel-Joannes" }, { "family_name": "Vanderbosch", "given_name": "Zachary P.", "orcid": "0000-0002-0853-3464", "clpid": "Vanderbosch-Zachary-P" }, { "family_name": "El-Badry", "given_name": "Kareem", "orcid": "0000-0002-6871-1752", "clpid": "El-Badry-Kareem" }, { "family_name": "Bellm", "given_name": "Eric C.", "orcid": "0000-0001-8018-5348", "clpid": "Bellm-Eric-C" }, { "family_name": "G\u00e4nsicke", "given_name": "Boris T.", "orcid": "0000-0002-2761-3005", "clpid": "G\u00e4nsicke-Boris-T" }, { "family_name": "Graham", "given_name": "Matthew J.", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "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": "Mr\u00f3z", "given_name": "Przemek", "orcid": "0000-0001-7016-1692", "clpid": "Mr\u00f3z-Przemek" }, { "family_name": "Riddle", "given_name": "Reed", "orcid": "0000-0002-0387-370X", "clpid": "Riddle-Reed-L" }, { "family_name": "Rusholme", "given_name": "Ben", "orcid": "0000-0001-7648-4142", "clpid": "Rusholme-Benjamin" } ], "abstract": "Magnetic CVs are luminous Galactic X-ray sources but have been difficult to find in purely optical surveys due to their lack of outburst behavior. The eROSITA telescope aboard the Spektr-RG (SRG) mission is conducting an all-sky X-ray survey and recently released the public eROSITA Final Equatorial Depth Survey (eFEDS) catalog. We crossmatched the eFEDS catalog with photometry from the Zwicky Transient Facility (ZTF) and discovered two new magnetic cataclysmic variables (CVs). We obtained high-cadence optical photometry and phase-resolved spectroscopy for each magnetic CV candidate and found them both to be polars. Among the newly discovered magnetic CVs is ZTFJ0850+0443, an eclipsing polar with orbital period P_(orb) = 1.72 hr, white dwarf mass M_(WD) = 0.81 \u00b1 0.08 M_\u2299 and accretion rate M\u02d9\u223c10\u207b\u00b9\u00b9 M_\u2299/yr. We suggest that ZTFJ0850+0443 is a low magnetic field strength polar, with B_(WD) \u2272 10 MG. We also discovered a non-eclipsing polar, ZTFJ0926+0105, with orbital period P_(orb) = 1.48 hr, magnetic field strength B_(WD)\u2273 26 MG, and accretion rate M\u02d9 \u223c10\u207b\u00b9\u00b2 M_\u2299/yr.", "doi": "10.48550/arXiv.2206.04714", "publisher": "arXiv", "publication_date": "2022-06-09" }, { "id": "authors:z46kt-e8w61", "collection": "authors", "collection_id": "z46kt-e8w61", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211213-224946143", "type": "monograph", "title": "Science with the Ultraviolet Explorer (UVEX)", "author": [ { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Harrison", "given_name": "Fiona A.", "orcid": "0000-0002-4226-8959", "clpid": "Harrison-F-A" }, { "family_name": "Grefenstette", "given_name": "Brian W.", "orcid": "0000-0002-1984-2932", "clpid": "Grefenstette-Brian-W" }, { "family_name": "Earnshaw", "given_name": "Hannah P.", "orcid": "0000-0001-5857-5622", "clpid": "Earnshaw-Hannah-P" }, { "family_name": "Andreoni", "given_name": "Igor", "orcid": "0000-0002-8977-1498" }, { "family_name": "Berg", "given_name": "Danielle A.", "orcid": "0000-0002-4153-053X" }, { "family_name": "Bloom", "given_name": "Joshua S.", "orcid": "0000-0002-7777-216X" }, { "family_name": "Cenko", "given_name": "S. Bradley", "orcid": "0000-0003-1673-970X" }, { "family_name": "Chornock", "given_name": "Ryan", "orcid": "0000-0002-7706-5668" }, { "family_name": "Christiansen", "given_name": "Jessie L.", "orcid": "0000-0002-8035-4778", "clpid": "Christiansen-Jessie-L" }, { "family_name": "Coughlin", "given_name": "Michael W.", "orcid": "0000-0002-8262-2924" }, { "family_name": "Criswell", "given_name": "Alexander Wuollet", "orcid": "0000-0002-9225-7756", "clpid": "Criswell-Alexander-W" }, { "family_name": "Darvish", "given_name": "Behnam", "orcid": "0000-0003-4919-9017", "clpid": "Darvish-Behnam" }, { "family_name": "Das", "given_name": "K.", "clpid": "Das-Kaustav-K" }, { "family_name": "De", "given_name": "Kishalay", "orcid": "0000-0002-8989-0542" }, { "family_name": "Dessart", "given_name": "Luc", "orcid": "0000-0003-0599-8407" }, { "family_name": "Dixon", "given_name": "Don" }, { "family_name": "Dorsman", "given_name": "Bas" }, { "family_name": "El-Badry", "given_name": "Kareem", "orcid": "0000-0002-6871-1752", "clpid": "El-Badry-Kareem" }, { "family_name": "Evans", "given_name": "Christopher" }, { "family_name": "Ford", "given_name": "K. E. Saavik", "orcid": "0000-0002-5956-851X" }, { "family_name": "Fremling", "given_name": "Christoffer", "orcid": "0000-0002-4223-103X", "clpid": "Fremling-Christoffer" }, { "family_name": "G\u00e4nsicke", "given_name": "Boris T.", "orcid": "0000-0002-2761-3005" }, { "family_name": "Gezari", "given_name": "Suvi", "orcid": "0000-0003-3703-5154" }, { "family_name": "G\u00f6tberg", "given_name": "Y.", "orcid": "0000-0002-6960-6911" }, { "family_name": "Green", "given_name": "Gregory M.", "orcid": "0000-0001-5417-2260" }, { "family_name": "Graham", "given_name": "Matthew J.", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "family_name": "Heida", "given_name": "Marianne", "orcid": "0000-0002-1082-7496" }, { "family_name": "Ho", "given_name": "Anna Y. Q.", "orcid": "0000-0002-9017-3567" }, { "family_name": "Jaodand", "given_name": "Amruta D.", "orcid": "0000-0002-3850-6651", "clpid": "Jaodand-Amruta-D" }, { "family_name": "Johns-Krull", "given_name": "Christopher M.", "orcid": "0000-0002-8828-6386" }, { "family_name": "Kasliwal", "given_name": "Mansi M.", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Lazzarini", "given_name": "Margaret", "orcid": "0000-0003-3252-352X", "clpid": "Lazzarini-Margaret" }, { "family_name": "Lu", "given_name": "Wenbin", "orcid": "0000-0002-1568-7461", "clpid": "Lu-Wenbin" }, { "family_name": "Margutti", "given_name": "Raffaella", "orcid": "0000-0003-4768-7586" }, { "family_name": "Martin", "given_name": "D. Christopher", "orcid": "0000-0002-8650-1644", "clpid": "Martin-D-Christopher" }, { "family_name": "Masters", "given_name": "Daniel Charles", "clpid": "Masters-Daniel-C" }, { "family_name": "McKernan", "given_name": "Barry", "orcid": "0000-0002-9726-0508" }, { "family_name": "Nissanke", "given_name": "Samaya M.", "orcid": "0000-0001-6573-7773" }, { "family_name": "Parazin", "given_name": "B.", "orcid": "0000-0002-3155-0385" }, { "family_name": "Perley", "given_name": "Daniel A.", "orcid": "0000-0001-8472-1996" }, { "family_name": "Phinney", "given_name": "E. Sterl", "orcid": "0000-0002-9656-4032", "clpid": "Phinney-E-S" }, { "family_name": "Piro", "given_name": "Anthony L.", "orcid": "0000-0001-6806-0673" }, { "family_name": "Raaijmakers", "given_name": "G.", "orcid": "0000-0002-9397-786X" }, { "family_name": "Rodriguez", "given_name": "Antonio C.", "orcid": "0000-0003-4189-9668", "clpid": "Rodriguez-Antonio-C" }, { "family_name": "Senchyna", "given_name": "Peter", "orcid": "0000-0002-9132-6561" }, { "family_name": "Singer", "given_name": "Leo P.", "orcid": "0000-0001-9898-5597" }, { "family_name": "Spake", "given_name": "Jessica J.", "orcid": "0000-0002-5547-3775", "clpid": "Spake-Jessica-J" }, { "family_name": "Stassun", "given_name": "Keivan G.", "orcid": "0000-0002-3481-9052" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-Daniel" }, { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-Harry-I" }, { "family_name": "Weisz", "given_name": "Daniel R.", "orcid": "0000-0002-6442-6030" }, { "family_name": "Yao", "given_name": "Yuhan", "orcid": "0000-0001-6747-8509", "clpid": "Yao-Yuhan" } ], "abstract": "The Ultraviolet Explorer (UVEX) will undertake a synoptic survey of the entire sky in near-UV (NUV) and far-UV (FUV) bands, probing the dynamic FUV and NUV universe, as well as perform a modern, all-sky imaging survey that reaches >50 times deeper than GALEX. Combined with a powerful broadband spectroscopic capability and timely response to target of opportunity discoveries, UVEX will address fundamental questions from the NASA Astrophysics Roadmap and the Astro2020 Decadal Survey, enabling unique and important studies across the breadth of astrophysics. Imaging and spectroscopic surveys with UVEX will probe key aspects of the evolution of galaxies by understanding how star formation and stellar evolution at low metallicities affect the growth and evolution of low-metallicity, low-mass galaxies in the local universe. Such galaxies contain half the mass in the local universe, and are analogs for the first galaxies, but observed at distances that make them accessible to detailed study. The UVEX time-domain surveys and prompt spectroscopic follow-up capability will probe the environments, energetics, and emission processes in the early aftermaths of gravitational wave-discovered compact object mergers, discover hot, fast UV transients, and diagnose the early stages of explosive phenomena. UVEX will become a key community resource by filling a gap in the new generation of wide-field, sensitive optical and infrared surveys provided by the Rubin, Euclid, and Roman observatories. We discuss the scientific potential of UVEX, including unique studies UVEX will enable for studying exoplanet atmospheres, hot stars, explosive phenomena, black holes, and galaxy evolution.", "doi": "10.48550/arXiv.2111.15608", "publisher": "arXiv", "publication_date": "2021-11-30" } ]