Мақола

Red and Reddened: Ultraviolet through Near-infrared Observations of Type Ia Supernova 2017erp*

Peter J. BrownDepartment of Physics and Astronomy, Texas A&M University, 4242 TAMU, College Station, TX 77843, USA; [email protected]Griffin HosseinzadehCenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USASaurabh W. JhaDepartment of Physics and Astronomy, Rutgers the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854, USADavid SandSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAEthan VieiraDepartment of Aerospace Engineering, Texas A&M University, 4242 TAMU, College Station, TX 77843, USAXiaofeng WangPhysics Department/Tsinghua Center for Astrophysics, Tsinghua University; Beijing, 100084, People’s Republic of ChinaMi DaiDepartment of Physics and Astronomy, Rutgers the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854, USAKyle G. DettmanDepartment of Physics and Astronomy, Rutgers the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854, USAJeremy MouldARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), AustraliaSyed UddinObservatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USALifan WangDepartment of Physics and Astronomy, Texas A&M University, 4242 TAMU, College Station, TX 77843, USA; [email protected]Iair ArcaviThe School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, IsraelJoao BentoResearch School of Astronomy and Astrophysics, Mount Stromlo Observatory, Australian National University, Cotter Road, Weston, Creek, ACT, 2611, AustraliaChris R. BurnsObservatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USATiara DiamondGoddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USADaichi HiramatsuDepartment of Physics, University of California, Santa Barbara, Santa Barbara, CA, 93106-9530, USAD. Andrew HowellDepartment of Physics, University of California, Santa Barbara, Santa Barbara, CA, 93106-9530, USAE. Y. HsiaoDepartment of Physics, Florida State University, Tallahassee, FL 32306, USAG. H. MarionUniversity of Texas at Austin, 1 University Station C1400, Austin, TX, 78712-0259, USACurtis McCullyDepartment of Physics, University of California, Santa Barbara, Santa Barbara, CA, 93106-9530, USAPeter MilneSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAD. O. MirzaqulovUlugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Uzbekistan, Tashkent, 100052, UzbekistanAshley J. RuiterARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), AustraliaStefano ValentiDepartment of Physics, University of California, Davis, 1 Shields Avenue, Davis, CA 95616-5270, USADanfeng XiangPhysics Department/Tsinghua Center for Astrophysics, Tsinghua University; Beijing, 100084, People’s Republic of China

The Astrophysical Journaljournal2019en

ABI

Аннотация

Abstract We present space-based ultraviolet/optical photometry and spectroscopy with the Swift Ultra-Violet/Optical Telescope and Hubble Space Telescope ( HST ), respectively, along with ground-based optical photometry and spectroscopy and near-infrared spectroscopy of supernova SN 2017erp. The optical light curves and spectra are consistent with a normal SN Ia. Compared to previous photometric samples in the near-ultraviolet (NUV), SN 2017erp has UV colors that are redder than NUV-blue SNe Ia corrected to similar optical colors. The chromatic difference between SNe 2011fe and 2017erp is dominated by the intrinsic differences in the UV rather than the expected dust reddening. This chromatic difference is similar to the SALT2 color law, derived from rest-frame ultraviolet photometry of higher redshift SNe Ia. Differentiating between intrinsic UV diversity and dust reddening can have important consequences for determining cosmological distances with rest-frame ultraviolet photometry. This ultraviolet spectroscopic series is the first from HST of a normal, albeit reddened, NUV-red SN Ia and is important for analyzing SNe Ia with intrinsically redder NUV colors. We show model comparisons suggesting that metallicity could be the physical difference between NUV-blue and NUV-red SNe Ia, with emission peaks from reverse fluorescence near 3000 Å implying a factor of ∼10 higher metallicity in the upper layers of SN 2017erp compared to SN 2011fe. Metallicity estimates are very model dependent, however, and there are multiple effects in the UV. Further models and UV spectra of SNe Ia are needed to explore the diversity of SNe Ia, which show seemingly independent differences in the near-UV peaks and mid-UV flux levels.

Ҳали таржима қилинмаган

Мавзулар

Gamma-ray bursts and supernovae Astro and Planetary Science Astronomy and Astrophysical Research

Идентификаторлар

DOI: 10.3847/1538-4357/ab1a3f

Иқтибослар ва манбалар

0 та иқтибос96 та фойдаланилган манба

Кўрсаткичлар — AkademScholar