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Carnegie Supernova Project-II: Near-infrared Spectroscopy of Stripped-envelope Core-collapse Supernovae

Shahbandeh, M. and Hsiao, E. Y. and Ashall, C. and Teffs, J. and Hoeflich, P. and Morrell, N. and Phillips, M. M. and Anderson, J. P. and Baron, E. and Burns, C. R. and Contreras, C. and Davis, S. and Diamond, T. R. and Folatelli, G. and Galbany, L. and Gall, C. and Hachinger, S. and Holmbo, S. and Karamehmetoglu, E. and Kasliwal, M. M. and Kirshner, R. P. and Krisciunas, K. and Kumar, S. and Lu, J. and Marion, G. H. and Mazzali, P. A. and Piro, A. L. and Sand, D. J. and Stritzinger, M. D. and Suntzeff, N. B. and Taddia, F. and Uddin, S. A. (2022) Carnegie Supernova Project-II: Near-infrared Spectroscopy of Stripped-envelope Core-collapse Supernovae. Astrophysical Journal, 925 (2). Art. No. 175. ISSN 0004-637X. doi:10.3847/1538-4357/ac4030.

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We present 75 near-infrared (NIR; 0.8−2.5 μm) spectra of 34 stripped-envelope core-collapse supernovae (SESNe) obtained by the Carnegie Supernova Project-II (CSP-II), encompassing optical spectroscopic Types IIb, Ib, Ic, and Ic-BL. The spectra range in phase from pre-maximum to 80 days past maximum. This unique data set constitutes the largest NIR spectroscopic sample of SESNe to date. NIR spectroscopy provides observables with additional information that is not available in the optical. Specifically, the NIR contains the strong lines of He i and allows a more detailed look at whether Type Ic supernovae are completely stripped of their outer He layer. The NIR spectra of SESNe have broad similarities, but closer examination through statistical means reveals a strong dichotomy between NIR "He-rich" and "He-poor" SNe. These NIR subgroups correspond almost perfectly to the optical IIb/Ib and Ic/Ic-BL types, respectively. The largest difference between the two groups is observed in the 2 μm region, near the He i λ2.0581 μm line. The division between the two groups is not an arbitrary one along a continuous sequence. Early spectra of He-rich SESNe show much stronger He i λ2.0581 μm absorption compared to the He-poor group, but with a wide range of profile shapes. The same line also provides evidence for trace amounts of He in half of our SNe in the He-poor group.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Shahbandeh, M.0000-0002-9301-5302
Hsiao, E. Y.0000-0003-1039-2928
Ashall, C.0000-0002-5221-7557
Teffs, J.0000-0001-8290-2881
Hoeflich, P.0000-0002-4338-6586
Morrell, N.0000-0003-2535-3091
Phillips, M. M.0000-0003-2734-0796
Anderson, J. P.0000-0003-0227-3451
Baron, E.0000-0001-5393-1608
Burns, C. R.0000-0003-4625-6629
Contreras, C.0000-0001-6293-9062
Davis, S.0000-0002-2806-5821
Diamond, T. R.0000-0002-0805-1908
Folatelli, G.0000-0001-5247-1486
Galbany, L.0000-0002-1296-6887
Gall, C.0000-0002-8526-3963
Hachinger, S.0000-0001-8341-1478
Holmbo, S.0000-0002-3415-322X
Karamehmetoglu, E.0000-0001-6209-838X
Kasliwal, M. M.0000-0002-5619-4938
Kirshner, R. P.0000-0002-1966-3942
Krisciunas, K.0000-0002-6650-694X
Kumar, S.0000-0001-8367-7591
Lu, J.0000-0002-3900-1452
Mazzali, P. A.0000-0001-6876-8284
Piro, A. L.0000-0001-6806-0673
Sand, D. J.0000-0003-4102-380X
Stritzinger, M. D.0000-0002-5571-1833
Suntzeff, N. B.0000-0002-8102-181X
Taddia, F.0000-0002-2387-6801
Uddin, S. A.0000-0002-9413-4186
Additional Information:© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 October 3; revised 2021 November 16; accepted 2021 November 17; published 2022 February 3. This paper includes data gathered with the 6.5 m Magellan Telescopes at Las Campanas Observatory, Chile. We are pleased to acknowledge the following individuals (in alphabetical order) for their assistance in obtaining the NIR spectroscopic data set: Y. Beletsky, T. Dupuy, R. Foley, L. W. Hsiao. We also thank the Las Campanas Observatory technical staff for their continued support over the years. The CSP-II has been supported by NSF grant Nos. AST-1008343, AST-1613426, AST-1613455, and AST-1613472. C.A. is supported by NASA grant No. 80NSSC19K1717 and NSF grant Nos. AST-1920392 and AST-1911074. J.T. is funded by the consolidated STFC grant No. R276106. L.G. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00. C.G. is supported by a Young Investor Grant (25501) from the VILLUM FONDEN. Time domain research by D.J.S. is also supported by NSF grant Nos. AST-1821987, 1813466, 1908972, & 2108032, and by the Heising-Simons Foundation under grant #2020-1864. M.D.S. is supported by grants from the VILLUM FONDEN (grant No. 28021) and the Independent Research Fund Denmark (IRFD; 8021-00170B). Software: firehose (Simcoe et al. 2013), SNID (Blondin & Tonry 2007), SNooPy (Burns et al. 2011), xtellcor (Vacca et al. 2003).
Group:Astronomy Department
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)R276106
Ramón y Cajal ProgrammeRYC2019-027683
Ministerio de Ciencia, Innovación y Universidades (MICIU)PID2020-115253GA-I00
Villum Foundation25501
Heising-Simons Foundation2020-1864
Villum Foundation28021
Independent Research Fund Denmark8021-00170B
Subject Keywords:Galactic and extragalactic astronomy; Core-collapse supernovae; Type Ib supernovae; Type Ic supernovae; Supernovae
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Galactic and extragalactic astronomy (563); Core-collapse supernovae (304); Type Ib supernovae (1729); Type Ic supernovae (1730); Supernovae (1668)
Record Number:CaltechAUTHORS:20220113-182233479
Persistent URL:
Official Citation:M. Shahbandeh et al 2022 ApJ 925 175
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:112875
Deposited By: George Porter
Deposited On:13 Jan 2022 22:42
Last Modified:08 Feb 2022 23:36

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