Search

Your search keyword '"Mockler, B"' showing total 17 results
Start Over Author "Mockler, B" Search Limiters Full Text
17 results on '"Mockler, B"'

1. Formation of Stripped Stars From Stellar Collisions in Galactic Nuclei

Author

Gibson, C., Kıroğlu, F., Lombardi Jr., J. C., Rose, S. C., Vanderzyden, H. D., Mockler, B., Gallegos-Garcia, M., Kremer, K., Ramirez-Ruiz, E., and Rasio, F. A.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Tidal disruption events (TDEs) are an important way to probe the properties of stellar populations surrounding supermassive black holes. Observed spectra of several TDEs, such as ASASSN-14li, show high nitrogen to carbon abundance ratios, leading to questions about their progenitors. Disrupting an intermediate- or high-mass star that has undergone CNO processing, increasing the nitrogen in its core, could lead to an enhanced nitrogen TDE. Galactic nuclei present a conducive environment for high-velocity stellar collisions that can lead to high mass loss, stripping the carbon- and hydrogen-rich envelopes of the stars and leaving behind the enhanced nitrogen cores. TDEs of these stripped stars may therefore exhibit even more extreme nitrogen enhancement. Using the smoothed particle hydrodynamics code StarSmasher, we provide a parameter space study of high-velocity stellar collisions involving intermediate-mass stars, analyzing the composition of the collision products. We conclude that high-velocity stellar collisions can form products that have abundance ratios similar to those observed in the motivating TDEs. Furthermore, we show that stars that have not experienced high CNO processing can yield low-mass collision products that retain even higher nitrogen to carbon abundance ratios. We analytically estimate the mass fallback for a typical TDE of several collision products to demonstrate consistency between our models and TDE observations. Lastly, we discuss how the extended collision products, with high central to average density ratios, can be related to repeated partial TDEs like ASASSN-14ko and G objects in the Galactic Center., Comment: 26 pages, 10 figures, 3 tables, submitted to ApJ

Published
2024

2. Evidence of a Massive Stellar Disruption in the X-ray Spectrum of ASASSN-14li

Author

Miller, J. M., Mockler, B., Ramirez-Ruiz, E., Draghis, P. A., Drake, J. J., Raymond, J., Reynolds, M. T., Xiang, X., Yun, S. -B., and Zoghbi, A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The proximity and duration of the tidal disruption event (TDE) ASASSN-14li led to the discovery of narrow, blue-shifted absorption lines in X-rays and UV. The gas seen in X-ray absorption is consistent with bound material close to the apocenter of elliptical orbital paths, or with a disk wind similar to those seen in Seyfert-1 active galactic nuclei. We present a new analysis of the deepest high-resolution XMM-Newton and Chandra spectra of ASASSN-14li. Driven by the relative strengths of He-like and H-like charge states, the data require [N/C] > 2.4, in qualitative agreement with UV spectral results. Flows of the kind seen in the X-ray spectrum of ASASSN-14li were not clearly predicted in simulations of TDEs; this left open the possibility that the observed absorption might be tied to gas released in prior AGN activity. However, the abundance pattern revealed in this analysis points to a single star rather than a standard AGN accretion flow comprised of myriad gas contributions. The simplest explanation of the data is likely that a moderately massive star (M ~ 3 Msun) with significant CNO processing was disrupted. An alternative explanation is that a lower mass star was disrupted that had previously been stripped of its envelope. We discuss the strengths and limitations of our analysis and these interpretations., Comment: Accepted for publication in ApJ Letters

Published
2023

3. Multiwavelength observations of the extraordinary accretion event AT2021lwx

Author

Wiseman, P., Wang, Y., Hönig, S., Castro-Segura, N., Clark, P., Frohmaier, C., Fulton, M. D., Leloudas, G., Middleton, M., Müller-Bravo, T. E., Mummery, A., Pursiainen, M., Smartt, S. J., Smith, K., Sullivan, M., Anderson, J. P., Pulido, J. A. Acosta, Charalampopoulos, P., Banerji, M., Dennefeld, M., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Ihanec, N., Kankare, E., Lawrence, A., Mockler, B., Moore, T., Nicholl, M., Onori, F., Petrushevska, T., Ragosta, F., Rest, S., Smith, M., Wevers, T., Carini, R., Chen, T. -W., Chambers, K., Gao, H., Huber, M., Inserra, C., Magnier, E., Makrygianni, L., Toy, M., Vincentelli, F., and Young, D. R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present observations from X-ray to mid-infrared wavelengths of the most energetic non-quasar transient ever observed, AT2021lwx. Our data show a single optical brightening by a factor $>100$ to a luminosity of $7\times10^{45}$ erg s$^{-1}$, and a total radiated energy of $1.5\times10^{53}$ erg, both greater than any known optical transient. The decline is smooth and exponential and the ultra-violet - optical spectral energy distribution resembles a black body with temperature $1.2\times10^4$ K. Tentative X-ray detections indicate a secondary mode of emission, while a delayed mid-infrared flare points to the presence of dust surrounding the transient. The spectra are similar to recently discovered optical flares in known active galactic nuclei but lack some characteristic features. The lack of emission for the previous seven years is inconsistent with the short-term, stochastic variability observed in quasars, while the extreme luminosity and long timescale of the transient disfavour the disruption of a single solar-mass star. The luminosity could be generated by the disruption of a much more massive star, but the likelihood of such an event occurring is small. A plausible scenario is the accretion of a giant molecular cloud by a dormant black hole of $10^8 - 10^9$ solar masses. AT2021lwx thus represents an extreme extension of the known scenarios of black hole accretion., Comment: 11 pages, 5 figures, Accepted for publication in MNRAS

Published
2023
Full Text
View/download PDF

4. 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
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., Comment: Accepted for publication in Nature Astronomy

Published
2022

5. The Young Supernova Experiment: Survey Goals, Overview, and Operations

Author

Jones, D. O., Foley, R. J., Narayan, G., Hjorth, J., Huber, M. E., Aleo, P. D., Alexander, K. D., Angus, C. R., Auchettl, K., Baldassare, V. F., Bruun, S. H., Chambers, K. C., Chatterjee, D., Coppejans, D. L., Coulter, D. A., DeMarchi, L., Dimitriadis, G., Drout, M. R., Engel, A., French, K. D., Gagliano, A., Gall, C., Hung, T., Izzo, L., Jacobson-Galán, W. V., Kilpatrick, C. D., Korhonen, H., Margutti, R., Raimundo, S. I., Ramirez-Ruiz, E., Rest, A., Rojas-Bravo, C., Siebert, M. R., Smartt, S. J., Smith, K. W., Terreran, G., Wang, Q., Wojtak, R., Agnello, A., Ansari, Z., Arendse, N., Baldeschi, A., Blanchard, P. K., Brethauer, D., Bright, J. S., Brown, J. S., deBoer, T. J. L., Dodd, S. A., Fairlamb, J. R., Grillo, C., Hajela, A., Hede, C., Kolborg, A. N., Law-Smith, J. A. P., Lin, C. -C., Magnier, E. A., Malanchev, K., Matthews, D., Mockler, B., Muthukrishna, D., Pan, Y. -C., Pfister, H., Ramanah, D. K., Rest, S., Sarangi, A., Schrøder, S. L., Stauffer, C., Stroh, M. C., Taggart, K. L., Tinyanont, S., and Wainscoat, R. J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Time domain science has undergone a revolution over the past decade, with tens of thousands of new supernovae (SNe) discovered each year. However, several observational domains, including SNe within days or hours of explosion and faint, red transients, are just beginning to be explored. Here, we present the Young Supernova Experiment (YSE), a novel optical time-domain survey on the Pan-STARRS telescopes. Our survey is designed to obtain well-sampled $griz$ light curves for thousands of transient events up to $z \approx 0.2$. This large sample of transients with 4-band light curves will lay the foundation for the Vera C. Rubin Observatory and the Nancy Grace Roman Space Telescope, providing a critical training set in similar filters and a well-calibrated low-redshift anchor of cosmologically useful SNe Ia to benefit dark energy science. As the name suggests, YSE complements and extends other ongoing time-domain surveys by discovering fast-rising SNe within a few hours to days of explosion. YSE is the only current four-band time-domain survey and is able to discover transients as faint $\sim$21.5 mag in $gri$ and $\sim$20.5 mag in $z$, depths that allow us to probe the earliest epochs of stellar explosions. YSE is currently observing approximately 750 square degrees of sky every three days and we plan to increase the area to 1500 square degrees in the near future. When operating at full capacity, survey simulations show that YSE will find $\sim$5000 new SNe per year and at least two SNe within three days of explosion per month. To date, YSE has discovered or observed 8.3% of the transient candidates reported to the International Astronomical Union in 2020. We present an overview of YSE, including science goals, survey characteristics and a summary of our transient discoveries to date., Comment: ApJ, in press; more information at https://yse.ucsc.edu/

Published
2020
Full Text
View/download PDF

6. The Spectral Evolution of at 2018dyb and the Presence of Metal Lines in Tidal Disruption Events

Author

Leloudas, G, Dai, L, Arcavi, I, Vreeswijk, PM, Mockler, B, Roy, R, Malesani, DB, Schulze, S, Wevers, T, Fraser, M, Ramirez-Ruiz, E, Auchettl, K, Burke, J, Cannizzaro, G, Charalampopoulos, P, Chen, TW, Cikota, A, Della Valle, M, Galbany, L, Gromadzki, M, Heintz, KE, Hiramatsu, D, Jonker, PG, Kostrzewa-Rutkowska, Z, Maguire, K, Mandel, I, Nicholl, M, Onori, F, Roth, N, Smartt, SJ, Wyrzykowski, L, and Young, DR

Subjects
astro-ph.HE, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present light curves and spectra of the tidal disruption event (TDE) ASASSN-18pg/AT 2018dyb spanning a period of one year. The event shows a plethora of strong emission lines, including the Balmer series, He ii, He i, and metal lines of O iii λ3760 and N iii λλ4100, 4640 (blended with He ii). The latter lines are consistent with originating from the Bowen fluorescence mechanism. By analyzing literature spectra of past events, we conclude that these lines are common in TDEs. The spectral diversity of optical TDEs is thus larger than previously thought and includes N-rich events besides H- and He-rich events. We study how the spectral lines evolve with time, by means of their width, relative strength, and velocity offsets. The velocity width of the lines starts at ∼13,000 km s-1 and decreases with time. The ratio of He ii to N iii increases with time. The same is true for ASASSN-14li, which has a very similar spectrum to AT 2018dyb but its lines are narrower by a factor of >2. We estimate a black hole mass of M BH = 3.3-2.0+5.0 × 106 Mo˙ by using the M-σ relation. This is consistent with the black hole mass derived using the MOSFiT transient fitting code. The detection of strong Bowen lines in the optical spectrum is an indirect proof for extreme ultraviolet and (reprocessed) X-ray radiation and favors an accretion origin for the TDE optical luminosity. A model where photons escape after multiple scatterings through a super-Eddington thick disk and its optically thick wind, viewed at an angle close to the disk plane, is consistent with the observations.

Published
2019

7. The fast, luminous ultraviolet transient AT2018cow: Extreme supernova, or disruption of a star by an intermediate-mass black hole?

Author

Perley, DA, Mazzali, PA, Yan, L, Cenko, SB, Gezari, S, Taggart, K, Blagorodnova, N, Fremling, C, Mockler, B, Singh, A, Tominaga, N, Tanaka, M, Watson, AM, Ahumada, T, Anupama, GC, Ashall, C, Becerra, RL, Bersier, D, Bhalerao, V, Bloom, JS, Butler, NR, Copperwheat, C, Coughlin, MW, De, K, Drake, AJ, Duev, DA, Frederick, S, González, JJ, Goobar, A, Heida, M, Ho, AYQ, Horst, J, Hung, T, Itoh, R, Jencson, JE, Kasliwal, MM, Kawai, N, Khanam, T, Kulkarni, SR, Kumar, B, Kumar, H, Kutyrev, AS, Lee, WH, Maeda, K, Mahabal, A, Murata, KL, Neill, JD, Ngeow, CC, Penprase, B, Pian, E, Quimby, R, Ramirez-Ruiz, E, Richer, MG, Romań-Zúñiga, CG, Sahu, DK, Srivastav, S, Socia, Q, Sollerman, J, Tachibana, Y, Taddia, F, Tinyanont, S, Troja, E, Ward, C, Wee, J, and Yu, PC

Subjects
Black hole, stars, supernovae: general, supernova: individual: AT2018cow, astro-ph.HE, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

Wide-field optical surveys have begun to uncover large samples of fast (trise ≲ 5 d), luminous (Mpeak < -18), blue transients. While commonly attributed to the breakout of a supernova shock into a dense wind, the great distances to the transients of this class found so far have hampered detailed investigation of their properties. We present photometry and spectroscopy from a comprehensive worldwide campaign to observe AT 2018cow (ATLAS 18qqn), the first fast-luminous optical transient to be found in real time at lowredshift. Our first spectra (10 days. The spectrum remains extremely hot throughout its evolution, and the photospheric radius contracts with time (receding below R < 1014 cm after 1 month). This behaviour does not match that of any known supernova, although a relativistic jet within a fallback supernova could explain some of the observed features. Alternatively, the transient could originate from the disruption of a star by an intermediate-mass black hole, although thiswould require long-lasting emission of highly super-Eddington thermal radiation. In either case, AT 2018cow suggests that the population of fast luminous transients represents a new class of astrophysical event. Intensive follow-up of this event in its late phases, and of any future events found at comparable distance, will be essential to better constrain their origins.

Published
2019

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

Author

Aleo, P. D., primary, Malanchev, K., additional, Sharief, S., additional, Jones, D. O., additional, Narayan, G., additional, Foley, R. J., additional, Villar, V. A., additional, Angus, C. R., additional, Baldassare, V. F., additional, Bustamante-Rosell, M. J., additional, Chatterjee, D., additional, Cold, C., additional, Coulter, D. A., additional, Davis, K. W., additional, Dhawan, S., additional, Drout, M. R., additional, Engel, A., additional, French, K. D., additional, Gagliano, A., additional, Gall, C., additional, Hjorth, J., additional, Huber, M. E., additional, Jacobson-Galán, W. V., additional, Kilpatrick, C. D., additional, Langeroodi, D., additional, Macias, P., additional, Mandel, K. S., additional, Margutti, R., additional, Matasić, F., additional, McGill, P., additional, Pierel, J. D. R., additional, Ramirez-Ruiz, E., additional, Ransome, C. L., additional, Rojas-Bravo, C., additional, Siebert, M. R., additional, Smith, K. W., additional, de Soto, K. M., additional, Stroh, M. C., additional, Tinyanont, S., additional, Taggart, K., additional, Ward, S. M., additional, Wojtak, R., additional, Auchettl, K., additional, Blanchard, P. K., additional, de Boer, T. J. L., additional, Boyd, B. M., additional, Carroll, C. M., additional, Chambers, K. C., additional, DeMarchi, L., additional, Dimitriadis, G., additional, Dodd, S. A., additional, Earl, N., additional, Farias, D., additional, Gao, H., additional, Gomez, S., additional, Grayling, M., additional, Grillo, C., additional, Hayes, E. E., additional, Hung, T., additional, Izzo, L., additional, Khetan, N., additional, Kolborg, A. N., additional, Law-Smith, J. A. P., additional, LeBaron, N., additional, Lin, C.-C., additional, Luo, Y., additional, Magnier, E. A., additional, Matthews, D., additional, Mockler, B., additional, O’Grady, A. J. G., additional, Pan, Y.-C., additional, Politsch, C. A., additional, Raimundo, S. I., additional, Rest, A., additional, Ridden-Harper, R., additional, Sarangi, A., additional, Schrøder, S. L., additional, Smartt, S. J., additional, Terreran, G., additional, Thorp, S., additional, Vazquez, J., additional, Wainscoat, R. J., additional, Wang, Q., additional, Wasserman, A. R., additional, Yadavalli, S. K., additional, Yarza, R., additional, and Zenati, Y., additional

Published
2023
Full Text
View/download PDF

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

Author

Aleo, P. D., Malanchev, K., Sharief, S., Jones, D. O., Narayan, G., Foley, R. J., Villar, V. A., Angus, C. R., Baldassare, V. F., Bustamante-Rosell, M. J., Chatterjee, D., Cold, C., Coulter, D. A., Davis, K. W., Dhawan, S., Drout, M. R., Engel, A., French, K. D., Gagliano, A., Gall, C., Hjorth, J., Huber, M. E., Jacobson-Galan, W. V., Kilpatrick, C. D., Langeroodi, D., Macias, P., Mandel, K. S., Margutti, R., Matasic, F., McGill, P., Pierel, J. D. R., Ramirez-Ruiz, E., Ransome, C. L., Rojas-Bravo, C., Siebert, M. R., Smith, K. W., de Soto, K. M., Stroh, M. C., Tinyanont, S., Taggart, K., Ward, S. M., Wojtak, R., Auchettl, K., Blanchard, P. K., de Boer, T. J. L., Boyd, B. M., Carroll, C. M., Chambers, K. C., DeMarchi, L., Dimitriadis, G., Dodd, S. A., Earl, N., Farias, D., Gao, H., Gomez, S., Grayling, M., Grillo, C., Hayes, E. E., Hung, T., Izzo, L., Khetan, N., Kolborg, A. N., Law-Smith, J. A. P., LeBaron, N., Lin, C. -c., Luo, Y., Magnier, E. A., Matthews, D., Mockler, B., O'Grady, A. J. G., Pan, Y. -c., Politsch, C. A., Raimundo, S. I., Rest, A., Ridden-Harper, R., Sarangi, A., Schroder, S. L., Smartt, S. J., Terreran, G., Thorp, S., Vazquez, J., Wainscoat, R. J., Wang, Q., Wasserman, A. R., Yadavalli, S. K., Yarza, R., Zenati, Y., Aleo, P. D., Malanchev, K., Sharief, S., Jones, D. O., Narayan, G., Foley, R. J., Villar, V. A., Angus, C. R., Baldassare, V. F., Bustamante-Rosell, M. J., Chatterjee, D., Cold, C., Coulter, D. A., Davis, K. W., Dhawan, S., Drout, M. R., Engel, A., French, K. D., Gagliano, A., Gall, C., Hjorth, J., Huber, M. E., Jacobson-Galan, W. V., Kilpatrick, C. D., Langeroodi, D., Macias, P., Mandel, K. S., Margutti, R., Matasic, F., McGill, P., Pierel, J. D. R., Ramirez-Ruiz, E., Ransome, C. L., Rojas-Bravo, C., Siebert, M. R., Smith, K. W., de Soto, K. M., Stroh, M. C., Tinyanont, S., Taggart, K., Ward, S. M., Wojtak, R., Auchettl, K., Blanchard, P. K., de Boer, T. J. L., Boyd, B. M., Carroll, C. M., Chambers, K. C., DeMarchi, L., Dimitriadis, G., Dodd, S. A., Earl, N., Farias, D., Gao, H., Gomez, S., Grayling, M., Grillo, C., Hayes, E. E., Hung, T., Izzo, L., Khetan, N., Kolborg, A. N., Law-Smith, J. A. P., LeBaron, N., Lin, C. -c., Luo, Y., Magnier, E. A., Matthews, D., Mockler, B., O'Grady, A. J. G., Pan, Y. -c., Politsch, C. A., Raimundo, S. I., Rest, A., Ridden-Harper, R., Sarangi, A., Schroder, S. L., Smartt, S. J., Terreran, G., Thorp, S., Vazquez, J., Wainscoat, R. J., Wang, Q., Wasserman, A. R., Yadavalli, S. K., Yarza, R., and Zenati, Y.

Abstract

We present the Young Supernova Experiment Data Release 1 (YSE DR1), comprised of processed multicolor PanSTARRS1 griz and Zwicky Transient Facility (ZTF) gr photometry of 1975 transients with host-galaxy associations, redshifts, spectroscopic and/or 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 approximate to 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 multisurvey 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 (similar to 71%) SNe Ia, 339 (similar to 23%) SNe II, and 96 (similar to 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.

Published
2023

10. Multiwavelength observations of the extraordinary accretion event AT2021lwx

Author

Wiseman, P, primary, Wang, Y, additional, Hönig, S, additional, Castro-Segura, N, additional, Clark, P, additional, Frohmaier, C, additional, Fulton, M D, additional, Leloudas, G, additional, Middleton, M, additional, Müller-Bravo, T E, additional, Mummery, A, additional, Pursiainen, M, additional, Smartt, S J, additional, Smith, K, additional, Sullivan, M, additional, Anderson, J P, additional, Acosta Pulido, J A, additional, Charalampopoulos, P, additional, Banerji, M, additional, Dennefeld, M, additional, Galbany, L, additional, Gromadzki, M, additional, Gutiérrez, C P, additional, Ihanec, N, additional, Kankare, E, additional, Lawrence, A, additional, Mockler, B, additional, Moore, T, additional, Nicholl, M, additional, Onori, F, additional, Petrushevska, T, additional, Ragosta, F, additional, Rest, S, additional, Smith, M, additional, Wevers, T, additional, Carini, R, additional, Chen, T-W, additional, Chambers, K, additional, Gao, H, additional, Huber, M, additional, Inserra, C, additional, Magnier, E, additional, Makrygianni, L, additional, Toy, M, additional, Vincentelli, F, additional, and Young, D R, additional

Published
2023
Full Text
View/download PDF

11. Evidence for the Preferential Disruption of Moderately Massive Stars by Supermassive Black Holes

Author

Mockler, B, Twum, AA, Auchettl, K, Dodd, S, French, KD, Law-Smith, JAP, Ramirez-Ruiz, E, Mockler, B, Twum, AA, Auchettl, K, Dodd, S, French, KD, Law-Smith, JAP, and Ramirez-Ruiz, E

Abstract

Tidal disruption events (TDEs) provide a unique opportunity to probe the stellar populations around supermassive black holes (SMBHs). By combining light-curve modeling with spectral line information and knowledge about the stellar populations in the host galaxies, we are able to constrain the properties of the disrupted star for three TDEs. The TDEs in our sample have UV spectra, and measurements of the UV N iii to C iii line ratios enabled estimates of the nitrogen-to-carbon abundance ratios for these events. We show that the measured nitrogen line widths are consistent with originating from the disrupted stellar material dispersed by the central SMBH. We find that these nitrogen-to-carbon abundance ratios necessitate the disruption of moderately massive stars (≳1–2 M ⊙). We determine that these moderately massive disruptions are overrepresented by a factor of ≳102 when compared to the overall stellar population of the post-starburst galaxy hosts. This implies that SMBHs are preferentially disrupting higher mass stars, possibly due to ongoing top-heavy star formation in nuclear star clusters or to dynamical mechanisms that preferentially transport higher mass stars to their tidal radii.

Published
2022

12. The Young Supernova Experiment:Survey Goals, Overview, and Operations

Author

Jones, D. O., Foley, R. J., Narayan, G., Hjorth, J., Huber, M. E., Aleo, P. D., Alexander, K. D., Angus, C. R., Auchettl, K., Baldassare, V. F., Bruun, S. H., Chambers, K. C., Chatterjee, D., Coppejans, D. L., Coulter, D. A., DeMarchi, L., Dimitriadis, G., Drout, M. R., Engel, A., French, K. D., Gagliano, A., Gall, C., Hung, T., Izzo, L., Jacobson-Galan, W. V., Kilpatrick, C. D., Korhonen, H., Margutti, R., Raimundo, S. I., Ramirez-Ruiz, E., Rest, A., Rojas-Bravo, C., Siebert, M. R., Smartt, S. J., Smith, K. W., Terreran, G., Wang, Q., Wojtak, R., Agnello, A., Ansari, Z., Arendse, N., Baldeschi, A., Blanchard, P. K., Brethauer, D., Bright, J. S., Brown, J. S., Boer, T. J. L. de, Dodd, S. A., Fairlamb, J. R., Grillo, C., Hajela, A., Hede, C., Kolborg, A. N., Law-Smith, J. A. P., Lin, C. -C., Magnier, E. A., Malanchev, K., Matthews, D., Mockler, B., Muthukrishna, D., Pan, Y. -C., Pfister, H., Ramanah, D. K., Rest, S., Sarangi, A., Schroder, S. L., Stauffer, C., Stroh, M. C., Taggart, K. L., Tinyanont, S., Wainscoat, R. J., Jones, D. O., Foley, R. J., Narayan, G., Hjorth, J., Huber, M. E., Aleo, P. D., Alexander, K. D., Angus, C. R., Auchettl, K., Baldassare, V. F., Bruun, S. H., Chambers, K. C., Chatterjee, D., Coppejans, D. L., Coulter, D. A., DeMarchi, L., Dimitriadis, G., Drout, M. R., Engel, A., French, K. D., Gagliano, A., Gall, C., Hung, T., Izzo, L., Jacobson-Galan, W. V., Kilpatrick, C. D., Korhonen, H., Margutti, R., Raimundo, S. I., Ramirez-Ruiz, E., Rest, A., Rojas-Bravo, C., Siebert, M. R., Smartt, S. J., Smith, K. W., Terreran, G., Wang, Q., Wojtak, R., Agnello, A., Ansari, Z., Arendse, N., Baldeschi, A., Blanchard, P. K., Brethauer, D., Bright, J. S., Brown, J. S., Boer, T. J. L. de, Dodd, S. A., Fairlamb, J. R., Grillo, C., Hajela, A., Hede, C., Kolborg, A. N., Law-Smith, J. A. P., Lin, C. -C., Magnier, E. A., Malanchev, K., Matthews, D., Mockler, B., Muthukrishna, D., Pan, Y. -C., Pfister, H., Ramanah, D. K., Rest, S., Sarangi, A., Schroder, S. L., Stauffer, C., Stroh, M. C., Taggart, K. L., Tinyanont, S., and Wainscoat, R. J.

Abstract

Time-domain science has undergone a revolution over the past decade, with tens of thousands of new supernovae (SNe) discovered each year. However, several observational domains, including SNe within days or hours of explosion and faint, red transients, are just beginning to be explored. Here we present the Young Supernova Experiment (YSE), a novel optical time-domain survey on the Pan-STARRS telescopes. Our survey is designed to obtain well-sampled griz light curves for thousands of transient events up to z 0.2. This large sample of transients with four-band light curves will lay the foundation for the Vera C. Rubin Observatory and the Nancy Grace Roman Space Telescope, providing a critical training set in similar filters and a well-calibrated low-redshift anchor of cosmologically useful SNe Ia to benefit dark energy science. As the name suggests, YSE complements and extends other ongoing time-domain surveys by discovering fast-rising SNe within a few hours to days of explosion. YSE is the only current four-band time-domain survey and is able to discover transients as faint as similar to 21.5 mag in gri and similar to 20.5 mag in z, depths that allow us to probe the earliest epochs of stellar explosions. YSE is currently observing approximately 750 deg(2) of sky every 3 days, and we plan to increase the area to 1500 deg(2) in the near future. When operating at full capacity, survey simulations show that YSE will find similar to 5000 new SNe per year and at least two SNe within 3 days of explosion per month. To date, YSE has discovered or observed 8.3% of the transient candidates reported to the International Astronomical Union in 2020. We present an overview of YSE, including science goals, survey characteristics, and a summary of our transient discoveries to date.

Published
2021

13. The Young Supernova Experiment: Survey Goals, Overview, and Operations

Author

Jones, D. O., primary, Foley, R. J., additional, Narayan, G., additional, Hjorth, J., additional, Huber, M. E., additional, Aleo, P. D., additional, Alexander, K. D., additional, Angus, C. R., additional, Auchettl, K., additional, Baldassare, V. F., additional, Bruun, S. H., additional, Chambers, K. C., additional, Chatterjee, D., additional, Coppejans, D. L., additional, Coulter, D. A., additional, DeMarchi, L., additional, Dimitriadis, G., additional, Drout, M. R., additional, Engel, A., additional, French, K. D., additional, Gagliano, A., additional, Gall, C., additional, Hung, T., additional, Izzo, L., additional, Jacobson-Galán, W. V., additional, Kilpatrick, C. D., additional, Korhonen, H., additional, Margutti, R., additional, Raimundo, S. I., additional, Ramirez-Ruiz, E., additional, Rest, A., additional, Rojas-Bravo, C., additional, Siebert, M. R., additional, Smartt, S. J., additional, Smith, K. W., additional, Terreran, G., additional, Wang, Q., additional, Wojtak, R., additional, Agnello, A., additional, Ansari, Z., additional, Arendse, N., additional, Baldeschi, A., additional, Blanchard, P. K., additional, Brethauer, D., additional, Bright, J. S., additional, Brown, J. S., additional, Boer, T. J. L. de, additional, Dodd, S. A., additional, Fairlamb, J. R., additional, Grillo, C., additional, Hajela, A., additional, Cold, C., additional, Kolborg, A. N., additional, Law-Smith, J. A. P., additional, Lin, C.-C., additional, Magnier, E. A., additional, Malanchev, K., additional, Matthews, D., additional, Mockler, B., additional, Muthukrishna, D., additional, Pan, Y.-C., additional, Pfister, H., additional, Ramanah, D. K., additional, Rest, S., additional, Sarangi, A., additional, Schrøder, S. L., additional, Stauffer, C., additional, Stroh, M. C., additional, Taggart, K. L., additional, Tinyanont, S., additional, and Wainscoat, R. J., additional

Published
2021
Full Text
View/download PDF

14. Combined fit of spectrum and composition data as measured by the Pierre Auger Observatory (vol 4, 038, 2017)

Author

Aab, A., Abreu, P., Aglietta, M., Samarai, Al, Albuquerque, I., Allekotte, I. F. M., Almela, I., Alvarez, Castillo, Alvarez-Muniz, J., Anastasi, Jessica, Anchordoqui, G. A., Rada, B., Ringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. M., Balaceanu, A., Barreira, Luz, Beatty, R. J., Becker, J. J., Bellido, K. H., Berat, J. A., Bertaina, C., Bertou, M. E., Biermann, X., Billoir, P. L., Biteau, P., Blaess, J., Blanco, S. G., Blazek, A., Bleve, J., Bohacova, C., Boncioli, M., Bonifazi, D., Borodai, C., Botti, N., Brack, A. M., Brancus, J., Bretz, I., Bridgeman, T., Briechle, A., Buchholz, F. L., Bueno, P., Buitink, A., Buscemi, S., Caballero-Mora, M., Caccianiga, K. S., Cancio, L., Canfora, A., Caramete, F., Caruso, L., Castellina, R., Cataldi, Alessia, Cazon, G., Chavez, L., Chinellato, A. G., Chudoba, J. A., Clay, J., Colalillo, R. W., Coleman, R., Collica, A., Coluccia, L., Conceicao, M. R., Contreras, R., Cooper, F., Coutu, M. J., Covault, S., Cronin, C. E., D'Amico, J., Daniel, S., Dasso, B., Daumiller, S., Dawson, K., B. R., Almeida, De, Costa, ROSANNA MARIA STEFANIA, Jong, De, S. J., Mauro, De, de Mello Neto, J. R. T., Mitri, De, Oliveira, De, Souza, De, Debatin, V., Deligny, J., DI GIULIO, Augusto, Matteo, Di, Diaz, Castro, Diogo, M. L., Dobrigkeit, F., D'Olivo, C., Dorosti, J. C., Dos, Anjos, Dova, R. C., Dundovic, M. T., Ebr, A., Engel, J., Erdmann, R., Erfani, M., Escobar, M., Espadanal, C. O., Etchegoyen, J., Falcke, A., Farrar, H., Fauth, G., Fazzini, A. C., Fick, N., Figueira, B., Filipcic, J. M., Fratu, A., Freire, O., Fujii, M. M., Fuster, T., Gaior, A., Garcia, R., Garcia-Pinto, B., Gate, D., Gemmeke, F., Gherghel-Lascu, H., Ghia, A., Giaccari, P. L., Giammarchi, U., Giller, M., LAS CASAS, Maria Carmela, Glaser, D. G., Golup, C., Gomez, Berisso, Gomez, Vitale, Gonzalez, P. F., Gorgi, N., Gorham, A., Grillo, P., Grubb, A. F., Guarino, T. D., Guedes, F., Hampel, G. P., Hansen, M. R., Harari, P., Harrison, D., Harton, T. A., Haungs, J. L., Hebbeker, A., Heck, T., Heimann, D., Herve, P., Hill, A. E., Hojvat, G. C., Holt, C., Homola, E., Hor, P., J. R., El, Horvath, P., Hrabovsky, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., J, T, Jansen, I., Johnsen, S., Josebachuili, J. A., Kaapa, M., Kambeitz, A., Kampert, O., Katkov, K. H., Keilhauer, I., Kemp, B., Kemp, E., Kieckhafer, J., Klages, R. M., Kleifges, H. O., Kleinfeller, M., Krause, J., Krohm, R., Kuempel, N., Mezek, D., Kukec, G., Kunka, N., Awad, Kuotb, A., Lahurd, D., Lauscher, M., Legumina, R., Leigui de Oliveira, Letessier-Selvon, M. A., Lhenry-Yvon, A., Link, I., Lopes, K., Lopez, L., Lopez, Casado, Luce, A., Lucero, Q., Malacari, A., Mallamaci, M., AYSAR M. M., Yasin, At, D., Mantsch, P., Mariazzi, A. G., Maris, I. C., Marsella, G., Martello, D., Martinez, H., Martinez, Bravo, Masias, Meza, Mathes, J. J., Mathys, H. J., Matthews, S., Matthews, J., Matthiae, J. A. J., Mayotte, G., Mazur, E., Medina, P. O., Medina-Tanco, C., Melo, G., Menshikov, D., Micheletti, A., Middendorf, M. I., Minaya, L., Miramonti, I. A., Mitrica, L., Mockler, B., Mollerach, D., Montanet, S., Morello, F., Mostafa, C., Mueller, M., Mueller, A. L., Muller, G., Mueller, M. A., Mussa, S., Naranjo, R., Nellen, I., Nguyen, L., Niculescu-Oglinzanu, P. H., Niechciol, M., Niemietz, M., Niggemann, L., Nitz, T., Nosek, D., Novotny, D., Nozka, V., Nunez, H., Ochilo, L. A., Oikonomou, L., Olinto, F., Palatka, A., Pallotta, M., Papenbreer, J., Parente, P., Parra, G., Paul, A., Pech, T., Pedreira, M., Pekala, F., Pelayo, J., Pena-Rodriguez, R., Pereira, J., Perlin, L. A. S., Perrone, M., Peters, L., Petrera, C., Phuntsok, S., Piegaia, J., Pierog, R., Pieroni, T., Pimenta, P., Pirronello, SILVIA MARIA GRAZIA, Platino, V., Plum, M., Porowski, M., Prado, C., Privitera, R. R., Prouza, P., Quel, M., Querchfeld, E. J., Quinn, S., Ramos-Pollan, S., Rautenberg, R., Ravignani, J., Revenu, D., Ridky, B., Risse, J., Ristori, M., Rizi, P., Rodrigues de Carvalho, Rodriguez, Fern, Ez, G., Rodriguez, Rojo, Rogozin, J., Roncoroni, D., Roth, M. J., Roulet, M., Rovero, E., Ruehl, A. C., Saffi, P., Saftoiu, S. J., Salamida, A., Salazar, F., Saleh, H., Greus, A., Salesa, F., Salina, G., Sanchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento, C. A., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovanek, P., Schroeder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Smialkowski, A., Smida, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Stanca, D., Stanic, S., Stasielak, J., Stassi, P., Strafella, F., Suarez, F., Suarez, Duran, Sudholz, M., Suomijarvi, T., Supanitsky, T., Swain, A. D., Szadkowski, J., Taboada, Z., Taborda, A., Tapia, O. A., Theodoro, A., Timmermans, V. M., Todero, Peixoto, Tomankova, C. J., Tome, L., Torralba, Elipe, Travnicek, G., Trini, P., Ulrich, M., Unger, R., Urban, M., Valdes, Galicia, Valino, J. F., Valore, I., Van, Aar, Van, Bodegom, van den Berg, A. M., Van, Vliet, BONILLA VARELA, Adelaida, Vargas, Cardenas, Varner, B., Vazquez, G., Vazquez, J. R., Veberic, R. A., Vergara, Quispe, Verzi, I. D., Vicha, V., Villasenor, J., Vorobiov, L., Wahlberg, S., Wainberg, H., Walz, O., Watson, D., Weber, A. A., Weindl, M., Wiencke, A., Wilczynski, L., Winchen, H., Wirtz, T., Wittkowski, M., Wundheiler, D., Yang, B., Yelos, L., Yushkov, D., Zas, A., Zavrtanik, E., Zavrtanik, D., Zepeda, M., Zimmermann, A., Ziolkowski, B., Zong, M., Zong, Z., and Pierre Auger Collaboration

Published
2018

15. 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
Full Text
View/download PDF

16. An Early-Time Optical and Ultraviolet Excess in the type-Ic SN 2020oi

Author

Alexander Gagliano, Luca Izzo, Charles D. Kilpatrick, Brenna Mockler, Wynn Vicente Jacobson-Galán, Giacomo Terreran, Georgios Dimitriadis, Yossef Zenati, Katie Auchettl, Maria R. Drout, Gautham Narayan, Ryan J. Foley, R. Margutti, Armin Rest, D. O. Jones, Christian Aganze, Patrick D. Aleo, Adam J. Burgasser, D. A. Coulter, Roman Gerasimov, Christa Gall, Jens Hjorth, Chih-Chun Hsu, Eugene A. Magnier, Kaisey S. Mandel, Anthony L. Piro, César Rojas-Bravo, Matthew R. Siebert, Holland Stacey, Michael Cullen Stroh, Jonathan J. Swift, Kirsty Taggart, Samaporn Tinyanont, Gagliano, A [0000-0003-4906-8447], Izzo, L [0000-0001-9695-8472], Kilpatrick, CD [0000-0002-5740-7747], Mockler, B [0000-0001-6350-8168], Jacobson-Galán, WV [0000-0003-1103-3409], Terreran, G [0000-0003-0794-5982], Dimitriadis, G [0000-0001-9494-179X], Auchettl, K [0000-0002-4449-9152], Drout, MR [0000-0001-7081-0082], Narayan, G [0000-0001-6022-0484], Foley, RJ [0000-0002-2445-5275], Margutti, R [0000-0003-4768-7586], Rest, A [0000-0002-4410-5387], Jones, DO [0000-0002-6230-0151], Aganze, C [0000-0003-2094-9128], Aleo, PD [0000-0002-6298-1663], Burgasser, AJ [0000-0002-6523-9536], Coulter, DA [0000-0003-4263-2228], Gerasimov, R [0000-0003-0398-639X], Gall, C [0000-0002-8526-3963], Hjorth, J [0000-0002-4571-2306], Hsu, CC [0000-0002-5370-7494], Magnier, EA [0000-0002-7965-2815], Mandel, KS [0000-0001-9846-4417], Piro, AL [0000-0001-6806-0673], Rojas-Bravo, C [0000-0002-7559-315X], Siebert, MR [0000-0003-2445-3891], Stroh, MC [0000-0002-3019-4577], Swift, JJ [0000-0002-9486-818X], Taggart, K [0000-0002-5748-4558], Tinyanont, S [0000-0002-1481-4676], and Apollo - University of Cambridge Repository

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, 5101 Astronomical Sciences, 13. Climate action, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, 5109 Space Sciences, Astrophysics - High Energy Astrophysical Phenomena, 51 Physical Sciences, 7. Clean energy, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present photometric and spectroscopic observations of Supernova 2020oi (SN 2020oi), a nearby ($\sim$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 $\delta t \approx 2.5$ days from the date of explosion in multi-band 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 $M_{\rm ej} = 0.81 \pm 0.03 M_{\odot}$, $E_{k}= 0.79 \pm 0.09 \times 10^{51} \rm{erg} \rm{s}^{-1}$, and $M_{\rm Ni56} = 0.08 \pm 0.02 M_{\odot}$. Inspection of the event's decline reveals the highest $\Delta m_{15,\rm{bol}}$ 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 (HST) 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 $M_{\rm ZAMS} \approx 9.5 \pm 1.0 M_{\odot}$, corresponding to an age of $27 \pm 7$ 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., Comment: 49 pages, 21 figures; accepted to ApJ

Published
2021

17. Deep reactive ion etched anti-reflection coatings for sub-millimeter silicon optics.

Author

Gallardo PA, Koopman BJ, Cothard NF, Bruno SM, Cortes-Medellin G, Marchetti G, Miller KH, Mockler B, Niemack MD, Stacey G, and Wollack EJ

Abstract

Refractive optical elements are widely used in millimeter and sub-millimeter (sub-mm) astronomical telescopes. High-resistivity silicon is an excellent material for dielectric lenses given its low loss tangent, high thermal conductivity, and high index of refraction. The high index of refraction of silicon causes a large Fresnel reflectance at the vacuum-silicon interface (up to 30%), which can be reduced with an anti-reflection (AR) coating. In this work, we report techniques for efficiently AR coating silicon at sub-mm wavelengths using deep reactive ion etching (DRIE) and bonding the coated silicon to another silicon optic. Silicon wafers of 100 mm diameter (1 mm thick) were coated and bonded using the silicon direct bonding technique at high temperature (1100°C). No glue is used in this process. Optical tests using a Fourier transform spectrometer show sub-percent reflections for a single-layer DRIE AR coating designed for use at 320 μm on a single wafer. Cryogenic (10 K) measurements of a bonded pair of AR-coated wafers also reached sub-percent reflections. A prototype two-layer DRIE AR coating to reduce reflections and increase bandwidth is presented, and plans for extending this approach are discussed.

Published
2017
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results