SIMBAD references

2020ApJ...898..166J - Astrophys. J., 898, 166-166 (2020/August-1)

SN 2019ehk: a double-peaked Ca-rich transient with luminous X-ray emission and shock-ionized spectral features.

JACOBSON-GALAN W.V., MARGUTTI R., KILPATRICK C.D., HIRAMATSU D., PERETS H., KHATAMI D., FOLEY R.J., RAYMOND J., YOON S.-C., BOBRICK A., ZENATI Y., GALBANY L., ANDREWS J., BROWN P.J., CARTIER R., COPPEJANS D.L., DIMITRIADIS G., DOBSON M., HAJELA A., HOWELL D.A., KUNCARAYAKTI H., MILISAVLJEVIC D., RAHMAN M., ROJAS-BRAVO C., SAND D.J., SHEPHERD J., SMARTT S.J., STACEY H., STROH M., SWIFT J.J., TERRERAN G., VINKO J., WANG X., ANDERSON J.P., BARON E.A., BERGER E., BLANCHARD P.K., BURKE J., COULTER D.A., DEMARCHI L., DERKACY J.M., FREMLING C., GOMEZ S., GROMADZKI M., HOSSEINZADEH G., KASEN D., KRISKOVICS L., McCULLY C., MULLER-BRAVO T.E., NICHOLL M., ORDASI A., PELLEGRINO C., PIRO A.L., PAL A., REN J., REST A., RICH R.M., SAI H., SARNECZKY K., SHEN K.J., SHORT P., SIEBERT M.R., STAUFFER C., SZAKATS R., ZHANG X., ZHANG J. and ZHANG K.

Abstract (from CDS):

We present panchromatic observations and modeling of the Calcium-rich supernova (SN) 2019ehk in the star-forming galaxy M100 (d ≃ 16.2 Mpc) starting 10 hr after explosion and continuing for ∼300 days. SN 2019ehk shows a double-peaked optical light curve peaking at t = 3 and 15 days. The first peak is coincident with luminous, rapidly decaying Swift-XRT-discovered X-ray emission (Lx~1041ergs–1 at 3 days; Lx ∝ t–3), and a Shane/Kast spectral detection of narrow Hα and He II emission lines (v ≃ 500 kms–1) originating from pre-existent circumstellar material (CSM). We attribute this phenomenology to radiation from shock interaction with extended, dense material surrounding the progenitor star at r < 1015 cm and the resulting cooling emission. We calculate a total CSM mass of ∼7 x 10–3 M (MHe/MH ≃6) with particle density n ≃ 109 cm–3. Radio observations indicate a significantly lower density n < 104 cm–3 at larger radii r > (0.1-1) x 1017 cm. The photometric and spectroscopic properties during the second light-curve peak are consistent with those of Ca-rich transients (rise-time of tr = 13.4 ± 0.210 days and a peak B-band magnitude of MB = -15.1 ± 0.200 mag). We find that SN 2019ehk synthesized (3.1 ± 0.11) x 10–2 M of 56Ni and ejected Mej = (0.72 ± 0.040)M total with a kinetic energy Ek = (1.8 ± 0.10) x 1050 erg. Finally, deep HST pre-explosion imaging at the SN site constrains the parameter space of viable stellar progenitors to massive stars in the lowest mass bin (∼10 M) in binaries that lost most of their He envelope or white dwarfs (WDs). The explosion and environment properties of SN 2019ehk further restrict the potential WD progenitor systems to low-mass hybrid HeCO WD+CO WD binaries.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Supernovae - White dwarf stars - Core-collapse supernovae - X-ray telescopes - Stellar mass loss - Stellar phenomena - Transient sources

Status at CDS : Large table(s) will be appraised for possible ingestion in VizieR.

Simbad objects: 32

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2021.04.17-13:11:14

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