المؤلفون: Raffaella Margutti, J. S. Bright, D. J. Matthews, D. L. Coppejans, K. D. Alexander, E. Berger, M. Bietenholz, R. Chornock, L. DeMarchi, M. R. Drout, T. Eftekhari, W. V. Jacobson-Galán, T. Laskar, D. Milisavljevic, K. Murase, M. Nicholl, C. M. B. Omand, M. Stroh, G. Terreran, B. A. VanderLey

المصدر: The Astrophysical Journal Letters, Vol 954, Iss 2, p L45 (2023)

مصطلحات موضوعية: Core-collapse supernovae, Extragalactic radio sources, Astrophysics, QB460-466

الوصف: We present the results from a multiyear radio campaign of the superluminous supernova (SLSN) SN 2017ens, which yielded the earliest radio detection of an SLSN to date at the age of ∼3.3 yr after explosion. SN 2017ens was not detected at radio frequencies in the first ∼300 days but reached L _ν ≈ 10 ^28 erg s ^−1 cm ^−2 Hz ^−1 at ν ∼ 6 GHz, ∼1250 days post explosion. Interpreting the radio observations in the context of synchrotron radiation from the supernova shock interaction with the circumstellar medium (CSM), we infer an effective mass-loss rate $\dot{M}\approx {10}^{-4}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}$ at r ∼ 10 ^17 cm from the explosion’s site, for a wind speed of v _w = 50–60 km s ^−1 as measured from optical spectra. These findings are consistent with the spectroscopic metamorphosis of SN 2017ens from hydrogen poor to hydrogen rich ∼190 days after explosion reported by Chen et al. SN 2017ens is thus an addition to the sample of hydrogen-poor massive progenitors that explode shortly after having lost their hydrogen envelope. The inferred circumstellar densities, implying a CSM mass up to ∼0.5 M _☉ , and low velocity of the ejection suggest that binary interactions (in the form of common-envelope evolution and subsequent envelope ejection) play a role in shaping the evolution of the stellar progenitors of SLSNe in the ≲500 yr preceding core collapse.

وصف الملف: electronic resource

العلاقة: https://doaj.org/toc/2041-8205Test

الوصول الحر: https://doaj.org/article/f7f078ac73cf4ef9a83c614548219151Test

المؤلفون: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink

المصدر: The Astrophysical Journal, Vol 959, Iss 2, p 125 (2023)

مصطلحات موضوعية: Binary stars, Close binary stars, Interacting binary stars, Early-type stars, Helium-rich stars, Helium burning, Astrophysics, QB460-466

الوصف: Massive stars (∼8–25 M _⊙ ) stripped of their hydrogen-rich envelopes via binary interaction are thought to be the main progenitors for merging neutron stars and stripped-envelope supernovae. We recently presented the discovery of the first set of such stripped stars in a companion paper. Here, we fit the spectra of 10 stars with new atmosphere models in order to constrain their stellar properties precisely. We find that the stellar properties align well with the theoretical expectations from binary evolution models for helium-core burning envelope-stripped stars. The fits confirm that the stars have high effective temperatures ( T _eff ∼ 50–100 kK), high surface gravities ( $\mathrm{log}g\sim $ 5), and hydrogen-poor/helium-rich surfaces ( X _H,surf ∼ 0–0.4) while showing for the first time a range of bolometric luminosities (10 ^3 –10 ^5 L _⊙ ), small radii (∼0.5–1 R _⊙ ), and low Eddington factors (Γ _e ∼ 0.006–0.4). Using these properties, we derive intermediate current masses (∼1–8 M _⊙ ), which suggest that their progenitors were massive stars (∼5–25 M _⊙ ) and that a subset will reach core-collapse, leaving behind neutron stars or black holes. Using the model fits, we also estimate the emission rates of ionizing photons for these stars, which agree well with previous model expectations. Further, by computing models for a range of mass-loss rates, we find that the stellar winds are weaker than predicted by any existing scheme ( ${\dot{M}}_{\mathrm{wind}}\lesssim {10}^{-9}$ M _⊙ yr ^−1 ). The properties of this first sample of intermediate-mass helium stars suggest they both contain progenitors of type Ib and IIb supernovae, and provide important benchmarks for binary evolution and population synthesis models.

وصف الملف: electronic resource

العلاقة: https://doaj.org/toc/1538-4357Test

الوصول الحر: https://doaj.org/article/a9625e8ed06e44da88cb99db67b71850Test

المؤلفون: 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, Young Supernova Experiment

المصدر: The Astrophysical Journal Supplement Series, Vol 266, Iss 1, p 9 (2023)

مصطلحات موضوعية: Supernovae, Surveys, Astronomy databases, Light curves, Light curve classification, Astrophysics, QB460-466

الوصف: 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 ≈ 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 (∼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.

وصف الملف: electronic resource

العلاقة: https://doaj.org/toc/0067-0049Test

الوصول الحر: https://doaj.org/article/0f1d0b0c0c094737bc61a1cd7b1d2518Test

المؤلفون: M Nicholl, P K Blanchard, E Berger, S Gomez, R Margutti, K D Alexander, J Guillochon, J Leja, R Chornock, B Snios, K Auchettl, A G Bruce, P Challis, D J D’Orazio, M R Drout, T Eftekhari, R J Foley, O Graur, C D Kilpatrick, A Lawrence, A L Piro, C Rojas-Bravo, N P Ross, P Short, S J Smartt, K W Smith, B Stalder

المصدر: Monthly Notices of the Royal Astronomical Society. 488(2):1878-1893

الوصول الحر: https://ntrs.nasa.gov/citations/20201765960518Test

المؤلفون: Raffaella Margutti, B. D. Metzger, R. Chornock, I. Vurm, N. Roth, B. W. Grefenstette, V. Savchenko, R. Cartier, J. F. Steiner, G. Terreran, G. Migliori, D. Milisavljevic, K. D. Alexander, M. Bietenholz, P. K. Blanchard, E. Bozzo, D. Brethauer, I. V. Chilingarian, D. L. Coppejans, L. Ducci, C. Ferrigno, W. Fong, D. GÖtz, C. Guidorzi, A. Hajela, K. Hurley, E. Kuulkers, P. Laurent, S. Mereghetti, M. Nicholl, D. Patnaude, P. Ubertini, J. Banovetz, N. Bartel, E. Berger, E. R. Coughlin, T. Eftekhari, D. D. Frederiks, A. V. Kozlova, T. Laskar, D. S. Svinkin, M. R. Drout, A. Macfadyen, K. Paterson

المساهمون: Margutti, Raffaella, Metzger, B. D., Chornock, R., Vurm, I., Roth, N., Grefenstette, B. W., Savchenko, V., Cartier, R., Steiner, J. F., Terreran, G., Migliori, G., Milisavljevic, D., Alexander, K. D., Bietenholz, M., Blanchard, P. K., Bozzo, E., Brethauer, D., Chilingarian, I. V., Coppejans, D. L., Ducci, L., Ferrigno, C., Fong, W., Götz, D., Guidorzi, C., Hajela, A., Hurley, K., Kuulkers, E., Laurent, P., Mereghetti, S., Nicholl, M., Patnaude, D., Ubertini, P., Banovetz, J., Bartel, N., Berger, E., Coughlin, E. R., Eftekhari, T., Frederiks, D. D., Kozlova, A. V., Laskar, T., Svinkin, D. S., Drout, M. R., Macfadyen, A., Paterson, K.

مصطلحات موضوعية: accretion, accretion disk, stars: black hole, supernovae: individual (AT 2018cow), X-rays: general

الوصف: We present the first extensive radio to γ-ray observations of a fast-rising blue optical transient, AT 2018cow, over its first ∼100 days. AT 2018cow rose over a few days to a peak luminosity L pk ∼ 4 × 10 44 erg s -1 , exceeding that of superluminous supernovae (SNe), before declining as L ∝ t -2 . Initial spectra at δt ≲ 15 days were mostly featureless and indicated large expansion velocities v ∼ 0.1c and temperatures reaching T ∼ 3 × 10 4 K. Later spectra revealed a persistent optically thick photosphere and the emergence of H and He emission features with v ∼ 4000 km s -1 with no evidence for ejecta cooling. Our broadband monitoring revealed a hard X-ray spectral component at E ≥ 10 keV, in addition to luminous and highly variable soft X-rays, with properties unprecedented among astronomical transients. An abrupt change in the X-ray decay rate and variability appears to accompany the change in optical spectral properties. AT 2018cow showed bright radio emission consistent with the interaction of a blast wave with v sh ∼ 0.1c with a dense environment ( for v w = 1000 km s -1 ). While these properties exclude 56 Ni-powered transients, our multiwavelength analysis instead indicates that AT 2018cow harbored a "central engine," either a compact object (magnetar or black hole) or an embedded internal shock produced by interaction with a compact, dense circumstellar medium. The engine released ∼10 50 -10 51.5 erg over ∼10 3 -10 5 s and resides within low-mass fast-moving material with equatorial-polar density asymmetry (M ej,fast ≲ 0.3 M). Successful SNe from low-mass H-rich stars (like electron-capture SNe) or failed explosions from blue supergiants satisfy these constraints. Intermediate-mass black holes are disfavored by the large environmental density probed by the radio observations.

وصف الملف: ELETTRONICO

العلاقة: info:eu-repo/semantics/altIdentifier/wos/WOS:000458043400018; volume:872; issue:1; firstpage:18-1; lastpage:18-32; numberofpages:32; journal:THE ASTROPHYSICAL JOURNAL; http://hdl.handle.net/11392/2401680Test; info:eu-repo/semantics/altIdentifier/scopus/2-s2.0-85062033314; https://iopscience.iop.org/article/10.3847/1538-4357/aafa01/pdfTest; https://iopscience.iop.org/article/10.3847/1538-4357/aafa01Test; https://arxiv.org/pdf/1810.10720.pdfTest

الإتاحة: https://doi.org/10.3847/1538-4357/aafa01Test
http://hdl.handle.net/11392/2401680Test
https://arxiv.org/pdf/1810.10720.pdfTest

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

المصدر: The Astrophysical Journal. 908(2):143

الوصول الحر: https://ntrs.nasa.gov/citations/31822922098123Test

المؤلفون: B. J. Shappee, T. W.-S. Holoien, M. R. Drout, K. Auchettl, M. D. Stritzinger, C. S. Kochanek, K. Z. Stanek, E. Shaya, G. Narayan, J. S. Brown, S. Bose, D. Bersier, J. Brimacombe, Ping Chen, Subo Dong, S. Holmbo, B. Katz, J. A. Munoz, R. L. Mutel, R. S. Post, J. L. Prieto, J. Shields, D. Tallon, T. A. Thompson, P. J. Vallely, S. Villanueva Jr, L. Denneau, H. Flewelling, A. N. Heinze, K. W. Smith, B. Stalder, J. L. Tonry, H. Weiland, T. Barclay, G. Barentsen, A. M. Cody, J. Dotson, F. Foerster, P. Garnavich, M. Gully-Santiago, C. Hedges, S. Howell, D. Kasen, S. Margheim, R. Mushotzky, A. Rest, B. E. Tucker, A. Villar, A. Zenteno, G. Beerman, R. Bjella, G. Castillo, J. Coughlin, B. Elsaesser, S. Flynn, R. Gangopadhyay, K. Griest, M. Hanley, J. Kampmeier, R. Kloetzel, L. Kohnert, C. Labonde, R. Larsen, K. A. Larson, K. M. McCalmont-Everton, C. McGinn, L. Migliorini, J. Moffatt, M. Muszynski, V. Nystrom, D. Osborne, M. Packard, C. A. Peterson, M. Redick, L. H. Reedy, S. E. Ross, B. Spencer, K. Steward, J. E. Van Cleve, J. Vinícius de Miranda-Cardoso, T. Weschler, A. Wheaton, J. Bulger, K. C. Chambers, H. A. Flewelling, M. E. Huber, T. B. Lowe, E. A. Magnier, A. S. B. Schultz, C. Z. Waters, M. Willman, E. Baron, Zhihao Chen, James M. Derkacy, Fang Huang, Linyi Li, Wenxiong Li, Xue Li, Jun Mo, Liming Rui, Hanna Sai, Lifan Wang, Lingzhi Wang, Xiaofeng Wang, Danfeng Xiang, Jicheng Zhang, Jujia Zhang, Kaicheng Zhang, Tianmeng Zhang, Xinghan Zhang, Xulin Zhao, P. J. Brown, J. J. Hermes, J. Nordin, S. Points, A. Sodor, G. M. Strampelli

المصدر: The Astrophysical Journal. 870(1)

مصطلحات موضوعية: Astrophysics

الوصف: On 2018 February 4.41, the All-Sky Automated Survey for SuperNovae (ASAS-SN) discovered ASASSN-18bt in the K2 Campaign 16 field. With a redshift of z=0.01098 and a peak apparent magnitude of B(max)=14.31, ASASSN-18bt is the nearest and brightest SNe Ia yet observed by the Kepler spacecraft. Here we present the discovery of ASASSN-18bt, the K2 light curve, and prediscovery data from ASAS-SN and the Asteroid Terrestrial-impact Last Alert System. The K2 early-time light curve has an unprecedented 30-minute cadence and photometric precision for an SN Ia light curve, and it unambiguously shows a ∼4 day nearly linear phase followed by a steeper rise. Thus, ASASSN-18bt joins a growing list of SNe Ia whose early light curves are not well described by a single power law. We show that a double-power-law model fits the data reasonably well, hinting that two physical processes must be responsible for the observed rise. However, we find that current models of the interaction with a nondegenerate companion predict an abrupt rise and cannot adequately explain the initial, slower linear phase. Instead, we find that existing published models with shallow 56Ni are able to span the observed behavior and, with tuning, may be able to reproduce the ASASSN-18bt light curve. Regardless, more theoretical work is needed to satisfactorily model this and other early-time SNe Ia light curves. Finally, we use Swift X-ray nondetections to constrain the presence of circumstellar material (CSM) at much larger distances and lower densities than possible with the optical light curve. For a constant-density CSM, these nondetections constrain ρ<4.5×10(exp 5)per cu.cm at a radius of 4×10(exp 15) cm from the progenitor star. Assuming a wind-like environment, we place mass loss limits of M˙ < 8 x 10(exp -6) M(ʘ)per yr for v(w)=100 km/s, ruling out some symbiotic progenitor systems. This work highlights the power of well-sampled early-time data and the need for immediate multiband, high-cadence follow-up for progress in understanding SNe Ia.

الوصول الحر: https://ntrs.nasa.gov/citations/20205004144Test

المؤلفون: Thomas Barclay, W. Li, X. Wang, J. Vinko, J. Mo, G. Hosseinzadeh, D. J. Sand, J. Zhang, H. Lin, T. Zhang, L. Wang, Z. Chen, D. Xiang, L. Rui, F. Huang, X. Li, X. Zhang, L. Li, E. Baron, J. M. Derkacy, X. Zhao, H. Sai, K. Zhang, D. A. Howell, C. McCully, I. Arcavi, S. Valenti, D. Hiramatsu, J. Burke, A. Rest, P. Garnavich, B. E. Tucker, G. Narayan, E. Shaya, S. Margheim, A. Zenteno, A. Villar, G. Dimitriadis, R. J. Foley, Y.-C. Pan, D. A. Coulter, O. D. Fox, S. W. Jha, D. O. Jones, D. N. Kasen, C. D. Kilpatrick, A. L. Piro, A. G. Riess, C. Rojas-Bravo, B. J. Shappee, T. W.-S. Holoien, K. Z. Stanek, M. R. Drout, K. Auchettl, C. S. Kochanek, J. S. Brown, S. Bose, D. Bersier, J. Brimacombe, P. Chen, S. Dong, S. Holmbo, J. A. Munoz, R. L. Mutel, R. S. Post, J. L. Prieto, J. Shields, D. Tallon, T. A. Thompson, P. J. Vallely, S. Villanueva Jr, S. J. Smartt, K. W. Smith, K. C. Chambers, H. A. Flewelling, M. E. Huber, E. A. Magnier, C. Z. Waters, A. S. B. Schultz, J. Bulger, T. B. Lowe, M. Willman, K. Sarneczky, A. Pal, J. C. Wheeler, A. Bodi, Zs. Bognar, B. Csak, B. Cseh, G. Csornyei, O. Hanyecz, B. Ignacz, Cs. Kalup, R. Konyves-Toth, L. Kriskovics, A. Ordasi, I. Rajmon5, A. Sodor, R. Szabo, R. Szakats, G. Zsidi, P. Milne, J. E. Andrews, N. Smith, C. Bilinski, P. J. Brown, J. Nordin, S. C. Williams, L. Galbany, J. Palmerio, I. M. Hook, C. Inserra, K. Maguire, Regis Cartier, A. Razza, C. P. Gutierrez, J. J. Hermes, J. S. Reding, B. C. Kaiser, J. L. Tonry, A. N. Heinze, L. Denneau, H. Weiland, B. Stalder, G. Barentsen, J Dotson, T Barclay, M Gully-Santiago, C. Hedges, A. M. Cody, S Howell, J. Coughlin, J. E. Van Cleve, J. Vinicius de Miranda Cardoso, K. A. Larson, K. M. McCalmont-Everton, C. A. Peterson, S. E. Ross, L. H. Reedy, D. Osborne, C. McGinn, L. Kohnert, L. Migliorini, A. Wheaton, B. Spencer, C. Labonde, G. Castillo, G. Beerman, K. Steward, M. Hanley, R. Larsen, R. Gangopadhyay, R. Kloetzel, T. Weschler, V. Nystrom, J. Moffatt, M. Redick, K. Griest, M. Packard, M. Muszynski, J. Kampmeier, R. Bjella, S. Flynn, B. Elsaesser

المصدر: The Astrophysical Journal. 870(1)

مصطلحات موضوعية: Astrophysics, Astronomy

الوصف: Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically confirmed Type Ia supernova (SN Ia) observed in the Kepler field. The Kepler data revealed an excess emission in its early light curve, allowing us to place interesting constraints on its progenitor system. Here we present extensive optical, ultraviolet, and nearinfrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3±0.3 days and Δ(m15)(B)=0.96±0.03 mag, but it seems to have bluer B−V colors. We construct the “UVOIR” bolometric light curve having a peak luminosity of 1.49×10(Exp 43) erg/s, from which we derive a nickel mass as 0.55±0.04M(ʘ) by fitting radiation diffusion models powered by centrally located 56Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of 56Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a nondegenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia but is characterized by prominent and persistent carbon absorption features. The CII features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in an SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.

الوصول الحر: https://ntrs.nasa.gov/citations/20205004176Test

المؤلفون: D. L. Coppejans, R. Margutti, G. Terreran, A. J. Nayana, E. R. Coughlin, T. Laskar, K. D. Alexander, M. Bietenholz, D. Caprioli, P. Chandra, M. R. Drout, D. Frederiks, C. Frohmaier, K. H Hurley, C. S. Kochanek, M. MacLeod, A. Meisner, P. E. Nugent, A. Ridnaia, D. J. Sand, D. Svinkin, C. Ward, S. Yang, A. Baldeschi, I. V. Chilingarian, Y. Dong, C. Esquivia, W. Fong, C. Guidorzi, P. Lundqvist, D. Milisavljevic, K. Paterson, D. E. Reichart, B. Shappee, M. C. Stroh, S. Valenti, B. A. Zauderer, B. Zhang

المصدر: The Astrophysical Journal Letters. 895(1):L23

الوصول الحر: https://ntrs.nasa.gov/citations/20875600418135Test

المؤلفون: Y. Cendes, M. R. Drout, L. Chomiuk, S. K. Sarbadhicary

المصدر: The Astrophysical Journal. 894(1):39

الوصول الحر: https://ntrs.nasa.gov/citations/66585452472760Test