分类： 天文学 >> 天文学 提交时间： 2023-02-19
Peter Hoeflich
Yi Yang
Dietrich Baade
Aleksandar Cikota
Justyn R. Maund
Divya Mishra
Ferdinando Patat
Kishore C. Patra
Lifan Wang
J. Craig Wheeler
Alexei V. Filippenko
Avishay Gal-Yam
Steve Schulze
摘要： Optical spectropolarimetry of the normal thermonuclear supernova SN2019np from -14.5 to +14.5 days relative to B-band maximum detected an intrinsic continuum polarization, p(cont), of 0.21+-0.09% at the first epoch. Between days -11.5 to +05, p(cont) remained about 0 and by day +14.5 was again significant at 0.19+-0.10%. Not considering the first epoch, the dominant axis of SiII(6355A) was roughly constant, staying close to the continuum until both rotated in opposite directions on day +14.5. Detailed radiation-hydrodynamical simulations produce a very steep density slope in the outermost ejecta so that the low first-epoch p(const) of about 0.2% nevertheless suggests a separate structure with an axis ratio of about 2 in the outer carbon-rich 3...5E-3 Mo. Large-amplitude fluctuations in the polarization profiles and a flocculent appearance of the polar diagram for the CaII near-infrared triplet (NIR3) may be related by a common origin. The temporal evolution of the polarization spectra agrees with an off-center delayed detonation. The late-time increase in polarization and the possible change in position angle are also consistent with an aspherical 56Ni core. The p(cont) and the absorptions due to Si II(6355A) and the CaII NIR3 form in the same region of the extended photosphere, with an interplay between line occultation and thermalization producing p. Small-scale polarization features may be due to small-scale structures, but many could be related to atomic patterns of the quasi-continuum; the hardly have an equivalent in the total-flux spectrum. We compare SN2019np to other SNe and develop future objectives and strategies for SNIa spectropolarimetry.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Yi Yang
Huirong Yan
Lifan Wang
J. Craig Wheeler
Dietrich Baade
Howard Isaacson
Aleksandar Cikota
Justyn R. Maund
Peter Hoeflich
Ferdinando Patat
Steven Giacalone
Malena Rice
Dakotah B. Tyler
Divya Mishra
Chris Ashall
Thomas G. Brink
Alexei V. Filippenko
Llíus Galbany
Kishore C. Patra
Melissa Shahbandeh
摘要： We report spectropolarimetric observations of the Type Ia supernova (SN) 2021rhu at four epochs: $-$7, +0, +36, and +79 days relative to its $B$-band maximum luminosity. A wavelength-dependent continuum polarization peaking at $3890 \pm 93$ Angstroms and reaching a level of $p_{\rm max}=1.78% \pm 0.02$% was found. The peak of the polarization curve is bluer than is typical in the Milky Way, indicating a larger proportion of small dust grains along the sightline to the SN. After removing the interstellar polarization, we found a pronounced increase of the polarization in the CaII near-infrared triplet, from $\sim$0.3% at day $-$7 to $\sim$2.5% at day +79. No temporal evolution in high-resolution flux spectra across the NaID and CaIIH&K features was seen from days +39 to +74, indicating that the late-time increase in polarization is intrinsic to the SN as opposed to being caused by scattering of SN photons in circumstellar or interstellar matter. We suggest that an explanation for the late-time rise of the CaII near-infrared triplet polarization may be the alignment of calcium atoms in a weak magnetic field through optical excitation/pumping by anisotropic radiation from the SN.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Viraj R. Karambelkar
Mansi M. Kasliwal
Nadejda Blagorodnova
Jesper Sollerman
Robert Aloisi
Shreya G. Anand
Igor Andreoni
Thomas G. Brink
Rachel Bruch
David Cook
Kaustav Kashyap Das
Kishalay De
Andrew Drake
Alexei V. Filippenko
Christoffer Fremling
George Helou
Anna Ho
Jacob Jencson
David Jones
Russ R. Laher
摘要： Luminous red novae (LRNe) are transients characterized by low luminosities and expansion velocities, and are associated with mergers or common envelope ejections in stellar binaries. Intermediate-luminosity red transients (ILRTs) are an observationally similar class with unknown origins, but generally believed to either be electron capture supernovae (ECSN) in super-AGB stars, or outbursts in dusty luminous blue variables (LBVs). In this paper, we present a systematic sample of 8 LRNe and 8 ILRTs detected as part of the Census of the Local Universe (CLU) experiment on the Zwicky Transient Facility (ZTF). The CLU experiment spectroscopically classifies ZTF transients associated with nearby ($<150$ Mpc) galaxies, achieving 80% completeness for m$_{r}<20$\,mag. Using the ZTF-CLU sample, we derive the first systematic LRNe volumetric-rate of 7.8$^{+6.5}_{-3.7}\times10^{-5}$ Mpc$^{-3}$ yr$^{-1}$ in the luminosity range $-16\leq$M$_{\rm{r}}$$\leq -11$ mag. We find that in this luminosity range, the LRN rate scales as dN/dL $\propto L^{-2.5\pm0.3}$ - significantly steeper than the previously derived scaling of $L^{-1.4\pm0.3}$ for lower luminosity LRNe (M$_{V}\geq-10$). The steeper power law for LRNe at high luminosities is consistent with the massive merger rates predicted by binary population synthesis models. We find that the rates of the brightest LRNe (M$_{r}\leq-13$ mag) are consistent with a significant fraction of them being progenitors of double compact objects (DCOs) that merge within a Hubble time. For ILRTs, we derive a volumetric rate of $2.6^{+1.8}_{-1.4}\times10^{-6}$ Mpc$^{-3}$yr$^{-1}$ for M$_{\rm{r}}\leq-13.5$, that scales as dN/dL $\propto L^{-2.5\pm0.5}$. This rate is $\approx1-5\%$ of the local core-collapse supernova rate, and is consistent with theoretical ECSN rate estimates.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
I. Irani
Ping Chen
Jonathan Morag
S. Schulze
A. Gal-Yam
Nora L. Strotjohann
Ofer Yaron
E. A. Zimmerman
Amir Sharon
Daniel A. Perley
J. Sollerman
Aaron Tohuvavohu
Kaustav K. Das
Mansi M. Kasliwal
Rachel Bruch
Thomas G. Brink
WeiKang Zheng
Kishore C. Patra
Sergiy S. Vasylyev
Alexei V. Filippenko
摘要： We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected <1 day after explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high-ionization C and O absorption features at velocities of 4,000 km s$^{-1}$, while its photospheric radius expands at 20,000 km s$^{-1}$, indicating a pre-existing distribution of expanding C/O material, likely ejected around 2 weeks before the explosion. After around 2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of 10,000 km s$^{-1}$, in agreement with the photospheric radius evolution. The optical light curves reach a second peak around t ~15 days. By t=60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong C II and [Ca II] emission with no detectable [O I] and marking this event as Ca-rich. The early behavior can be explained by $10^{-3}$ solar mass of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf-Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by a combination of interaction of the ejecta with the optically thin CSM and shock cooling (in the massive-star scenario), until the radioactive decay of $^{56}$Ni becomes the dominant power source. The observations can be explained by CSM that is optically thick to X-ray photons which are down converted, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from down-converted X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.
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