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3 results on '"Mockler, B"'

1. A fast rising tidal disruption event from a candidate intermediate mass black hole

Author

Angus, C. R., Baldassare, V. F., Mockler, B., Foley, R. J., Ramirez-Ruiz, E., Raimundo, S. I., French, K. D., Auchettl, K., Pfister, H., Gall, C., Hjorth, J., Drout, M. R., Alexander, K. D., Dimitriadis, G., Hung, T., Jones, D. O., Rest, A., Siebert, M. R., Taggart, K., Terreran, G., Tinyanont, S., Carroll, C. M., DeMarchi, L., Earl, N., Gagliano, A., Izzo, L., Villar, V. A., Zenati, Y., Arendse, N., Cold, C., de Boer, T. J. L., Chambers, K. C., Coulter, D. A., Khetan, N., Lin, C. C., Magnier, E. A., Rojas-Bravo, C., Wainscoat, R. J., and Wojtak, R.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

Massive black holes (BHs) at the centres of massive galaxies are ubiquitous. The population of BHs within dwarf galaxies, on the other hand, is evasive. Dwarf galaxies are thought to harbour BHs with proportionally small masses, including intermediate mass BHs, with masses $10^{2} < M_{BH} < 10^{6} M_{\odot}$. Identification of these systems has historically relied upon the detection of light emitted from accreting gaseous discs close to the BHs. Without this light, they are difficult to detect. Tidal disruption events (TDEs), the luminous flares produced when a star strays close to a BH and is shredded, are a direct way to probe massive BHs. The rise times of these flares theoretically correlate with the BH mass. Here we present AT2020neh, a fast rising TDE candidate, hosted by a dwarf galaxy. AT2020neh can be described by the tidal disruption of a main sequence star by a 10$^{4.7} - 10^{5.9} M_{\odot}$ BH. We find the observable rate of fast rising nuclear transients like AT2020neh to be rare, at $\lesssim 2 \times 10^{-8}$ events Mpc$^{-3}$ yr$^{-1}$. Finding non-accreting BHs in dwarf galaxies is important to determine how prevalent BHs are within these galaxies, and constrain models of BH formation. AT2020neh-like events may provide a galaxy-independent method of measuring IMBH masses., Accepted for publication in Nature Astronomy

Published
2022
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2. An Early-time Optical and Ultraviolet Excess in the Type-Ic SN 2020oi

Author

Gagliano, A, Izzo, L, Kilpatrick, CD, Mockler, B, Jacobson-Galán, WV, Terreran, G, Dimitriadis, G, Zenati, Y, Auchettl, K, Drout, MR, Narayan, G, Foley, RJ, Margutti, R, Rest, A, Jones, DO, Aganze, C, Aleo, PD, Burgasser, AJ, Coulter, DA, Gerasimov, R, Gall, C, Hjorth, J, Hsu, CC, Magnier, EA, Mandel, KS, Piro, AL, Rojas-Bravo, C, Siebert, MR, Stacey, H, Stroh, MC, Swift, JJ, Taggart, K, and Tinyanont, S

Subjects
13. Climate action, 5101 Astronomical Sciences, 5109 Space Sciences, 7. Clean energy, 51 Physical Sciences
Abstract

We present photometric and spectroscopic observations of Supernova 2020oi (SN 2020oi), a nearby (∼17 Mpc) type-Ic supernova (SN Ic) within the grand-design spiral M100. We undertake a comprehensive analysis to characterize the evolution of SN 2020oi and constrain its progenitor system. We detect flux in excess of the fireball rise model δ t ≈ 2.5 days from the date of explosion in multiband optical and UV photometry from the Las Cumbres Observatory and the Neil Gehrels Swift Observatory, respectively. The derived SN bolometric luminosity is consistent with an explosion with M ej = 0.81 ± 0.03 M ⊙, E k = 0.79 ± 0.09 × 1051 erg s−1, and M Ni56 = 0.08 ± 0.02 M ⊙. Inspection of the event’s decline reveals the highest Δm 15,bol reported for a stripped-envelope event to date. Modeling of optical spectra near event peak indicates a partially mixed ejecta comparable in composition to the ejecta observed in SN 1994I, while the earliest spectrum shows signatures of a possible interaction with material of a distinct composition surrounding the SN progenitor. Further, Hubble Space Telescope pre-explosion imaging reveals a stellar cluster coincident with the event. From the cluster photometry, we derive the mass and age of the SN progenitor using stellar evolution models implemented in the BPASS library. Our results indicate that SN 2020oi occurred in a binary system from a progenitor of mass M ZAMS ≈ 9.5 ± 1.0 M ⊙, corresponding to an age of 27 ± 7 Myr. SN 2020oi is the dimmest SN Ic event to date for which an early-time flux excess has been observed, and the first in which an early excess is unlikely to be associated with shock cooling.

3. The Young Supernova Experiment Data Release 1 (YSE DR1): Light Curves and Photometric Classification of 1975 Supernovae

Author

P. D. Aleo, K. Malanchev, S. Sharief, D. O. Jones, G. Narayan, R. J. Foley, V. A. Villar, C. R. Angus, V. F. Baldassare, M. J. Bustamante-Rosell, D. Chatterjee, C. Cold, D. A. Coulter, K. W. Davis, S. Dhawan, M. R. Drout, A. Engel, K. D. French, A. Gagliano, C. Gall, J. Hjorth, M. E. Huber, W. V. Jacobson-Galán, C. D. Kilpatrick, D. Langeroodi, P. Macias, K. S. Mandel, R. Margutti, F. Matasić, P. McGill, J. D. R. Pierel, E. Ramirez-Ruiz, C. L. Ransome, C. Rojas-Bravo, M. R. Siebert, K. W. Smith, K. M. de Soto, M. C. Stroh, S. Tinyanont, K. Taggart, S. M. Ward, R. Wojtak, K. Auchettl, P. K. Blanchard, T. J. L. de Boer, B. M. Boyd, C. M. Carroll, K. C. Chambers, L. DeMarchi, G. Dimitriadis, S. A. Dodd, N. Earl, D. Farias, H. Gao, S. Gomez, M. Grayling, C. Grillo, E. E. Hayes, T. Hung, L. Izzo, N. Khetan, A. N. Kolborg, J. A. P. Law-Smith, N. LeBaron, C.-C. Lin, Y. Luo, E. A. Magnier, D. Matthews, B. Mockler, A. J. G. O’Grady, Y.-C. Pan, C. A. Politsch, S. I. Raimundo, A. Rest, R. Ridden-Harper, A. Sarangi, S. L. Schrøder, S. J. Smartt, G. Terreran, S. Thorp, J. Vazquez, R. J. Wainscoat, Q. Wang, A. R. Wasserman, S. K. Yadavalli, R. Yarza, Y. Zenati, Aleo, PD [0000-0002-6298-1663], Malanchev, K [0000-0001-7179-7406], Sharief, S [0000-0002-0869-8760], Jones, DO [0000-0002-6230-0151], Narayan, G [0000-0001-6022-0484], Foley, RJ [0000-0002-2445-5275], Villar, VA [0000-0002-5814-4061], Angus, CR [0000-0002-4269-7999], Baldassare, VF [0000-0003-4703-7276], Bustamante-Rosell, MJ [0000-0003-0416-9818], Chatterjee, D [0000-0003-0038-5468], Cold, C [0000-0001-7666-1874], Coulter, DA [0000-0003-4263-2228], Davis, KW [0000-0002-5680-4660], Dhawan, S [0000-0002-2376-6979], Drout, MR [0000-0001-7081-0082], Engel, A [0000-0003-2348-483X], French, KD [0000-0002-4235-7337], Gagliano, A [0000-0003-4906-8447], Gall, C [0000-0002-8526-3963], Hjorth, J [0000-0002-4571-2306], Huber, ME [0000-0003-1059-9603], Jacobson-Galán, WV [0000-0002-3934-2644], Kilpatrick, CD [0000-0002-5740-7747], Langeroodi, D [0000-0001-5710-8395], Macias, P [0000-0002-9946-4635], Mandel, KS [0000-0001-9846-4417], Margutti, R [0000-0003-4768-7586], Matasić, F [0000-0001-5306-1948], McGill, P [0000-0002-1052-6749], Pierel, JDR [0000-0002-2361-7201], Ramirez-Ruiz, E [0000-0003-2558-3102], Ransome, CL [0000-0003-4175-4960], Rojas-Bravo, C [0000-0002-7559-315X], Siebert, MR [0000-0003-2445-3891], Smith, KW [0000-0001-9535-3199], De Soto, KM [0000-0002-9886-2834], Stroh, MC [0000-0002-3019-4577], Tinyanont, S [0000-0002-1481-4676], Taggart, K [0000-0002-5748-4558], Ward, SM [0000-0002-1763-2720], Wojtak, R [0000-0001-9666-3164], Auchettl, K [0000-0002-4449-9152], Blanchard, PK [0000-0003-0526-2248], De Boer, TJL [0000-0001-5486-2747], Boyd, BM [0000-0002-0622-1117], Carroll, CM [0000-0003-3574-2963], Chambers, KC [0000-0001-6965-7789], Demarchi, L [0000-0003-4587-2366], Dimitriadis, G [0000-0001-9494-179X], Dodd, SA [0000-0002-3696-8035], Earl, N [0000-0003-1714-7415], Farias, D [0000-0002-6886-269X], Gao, H [0000-0003-1015-5367], Gomez, S [0000-0001-6395-6702], Grayling, M [0000-0002-6741-983X], Grillo, C [0000-0002-5926-7143], Hayes, EE [0000-0003-3847-0780], Hung, T [0000-0002-9878-7889], Izzo, L [0000-0001-9695-8472], Khetan, N [0000-0003-2720-8904], Kolborg, AN [0000-0001-7364-4964], Law-Smith, JAP [0000-0001-8825-4790], Lin, CC [0000-0002-7272-5129], Luo, Y [0000-0002-4623-0683], Magnier, EA [0000-0002-7965-2815], Matthews, D [0000-0002-4513-3849], Mockler, B [0000-0001-6350-8168], O'Grady, AJG [0000-0002-7296-6547], Pan, YC [0000-0001-8415-6720], Politsch, CA [0000-0003-3727-9167], Raimundo, SI [0000-0002-6248-398X], Rest, A [0000-0002-4410-5387], Ridden-Harper, R [0000-0003-1724-2885], Sarangi, A [0000-0002-9820-679X], Schrøder, SL [0000-0003-1735-8263], Smartt, SJ [0000-0002-8229-1731], Terreran, G [0000-0003-0794-5982], Vazquez, J [0000-0003-1576-0830], Wainscoat, RJ [0000-0002-1341-0952], Wang, Q [0000-0001-5233-6989], Wasserman, AR [0000-0002-4186-6164], Yadavalli, SK [0000-0002-0840-6940], Yarza, R [0000-0003-0381-1039], Zenati, Y [0000-0002-0632-8897], and Apollo - University of Cambridge Repository

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), COSMOLOGICAL CONSTRAINTS, DARK ENERGY SURVEY, IA SUPERNOVAE, FOS: Physical sciences, Astronomy and Astrophysics, 5109 Space Sciences, MEDIUM-DEEP SURVEY, PAN-STARRS, I. OBSERVATIONS, Astrophysics - Solar and Stellar Astrophysics, CORE-COLLAPSE SUPERNOVAE, GALAXY REDSHIFT SURVEY, SUPERLUMINOUS SUPERNOVAE, Space and Planetary Science, IC SUPERNOVA, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, 51 Physical Sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), High-Energy Phenomena and Fundamental Physics
Abstract

We present the Young Supernova Experiment Data Release 1 (YSE DR1), comprised of processed multi-color Pan-STARRS1 (PS1) griz and Zwicky Transient Facility (ZTF) gr photometry of 1975 transients with host-galaxy associations, redshifts, spectroscopic/photometric classifications, and additional data products from 2019 November 24 to 2021 December 20. YSE DR1 spans discoveries and observations from young and fast-rising supernovae (SNe) to transients that persist for over a year, with a redshift distribution reaching z~0.5. We present relative SN rates from YSE's magnitude- and volume-limited surveys, which are consistent with previously published values within estimated uncertainties for untargeted surveys. We combine YSE and ZTF data, and create multi-survey SN simulations to train the ParSNIP and SuperRAENN photometric classification algorithms; when validating our ParSNIP classifier on 472 spectroscopically classified YSE DR1 SNe, we achieve 82% accuracy across three SN classes (SNe Ia, II, Ib/Ic) and 90% accuracy across two SN classes (SNe Ia, core-collapse SNe). Our classifier performs particularly well on SNe Ia, with high (>90%) individual completeness and purity, which will help build an anchor photometric SNe Ia sample for cosmology. We then use our photometric classifier to characterize our photometric sample of 1483 SNe, labeling 1048 (~71%) SNe Ia, 339 (~23%) SNe II, and 96 (~6%) SNe Ib/Ic. YSE DR1 provides a training ground for building discovery, anomaly detection, and classification algorithms, performing cosmological analyses, understanding the nature of red and rare transients, exploring tidal disruption events and nuclear variability, and preparing for the forthcoming Vera C. Rubin Observatory Legacy Survey of Space and Time., Accepted to ApJS; 64 pages; 35 figures; 10 tables

Published
2023
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