What We Learn from the X-Ray Grating Spectra of Nova SMC 2016

M. Orio, J. U. Ness, A. Dobrotka, E. Gatuzz, N. Ospina, E. Aydi, E. Behar, D. A.H. Buckley, S. Ciroi, M. Della Valle, M. Hernanz, M. Henze, J. P. Osborne, K. L. Page, T. Rauch, G. Sala, Sumner Starrfield, R. E. Williams, C. E. Woodward, P. Zemko

Research output: Contribution to journalArticle

1 Citation (Scopus)

Abstract

Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between days 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera, and the Low Energy Transmission Grating on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon, and sulfur on day 39, and oxygen, nitrogen, and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blueshifted, by about 1800 km s-1 on day 39 and up to 2100 km s-1 in the following observations. Spectral lines attributed to low-ionization potential transitions in the interstellar medium are also observed. Assuming the distance to the Small Magellanic Cloud, the bolometric luminosity exceeded the Eddington level for at least three months. A preliminary analysis with atmospheric models indicates an effective temperature of around 700,000 K on day 39, peaking at the later dates in the 850,000-900,000 K range, as expected for a ≃1.25 M o WD. We suggest a possible classification as an oxygen-neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show a large, aperiodic flux variability, which is not associated with spectral variability. We detected red noise, but did not find periodic or quasiperiodic modulations.

Original languageEnglish (US)
Article number164
JournalAstrophysical Journal
Volume862
Issue number2
DOIs
StatePublished - Aug 1 2018

Fingerprint

gratings (spectra)
Magellanic clouds
nitrogen
oxygen
x rays
neon
atmospheric models
carbon
XMM-Newton telescope
argon
ionization potentials
newton
light curve
line spectra
magnesium
calcium
ionization
sulfur
cameras
luminosity

Keywords

  • novae, cataclysmic variables
  • stars: abundances
  • stars: dwarf novae
  • stars: individual (N SMC 2016a)
  • X-rays: stars

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Orio, M., Ness, J. U., Dobrotka, A., Gatuzz, E., Ospina, N., Aydi, E., ... Zemko, P. (2018). What We Learn from the X-Ray Grating Spectra of Nova SMC 2016. Astrophysical Journal, 862(2), [164]. https://doi.org/10.3847/1538-4357/aacf06

What We Learn from the X-Ray Grating Spectra of Nova SMC 2016. / Orio, M.; Ness, J. U.; Dobrotka, A.; Gatuzz, E.; Ospina, N.; Aydi, E.; Behar, E.; Buckley, D. A.H.; Ciroi, S.; Della Valle, M.; Hernanz, M.; Henze, M.; Osborne, J. P.; Page, K. L.; Rauch, T.; Sala, G.; Starrfield, Sumner; Williams, R. E.; Woodward, C. E.; Zemko, P.

In: Astrophysical Journal, Vol. 862, No. 2, 164, 01.08.2018.

Research output: Contribution to journalArticle

Orio, M, Ness, JU, Dobrotka, A, Gatuzz, E, Ospina, N, Aydi, E, Behar, E, Buckley, DAH, Ciroi, S, Della Valle, M, Hernanz, M, Henze, M, Osborne, JP, Page, KL, Rauch, T, Sala, G, Starrfield, S, Williams, RE, Woodward, CE & Zemko, P 2018, 'What We Learn from the X-Ray Grating Spectra of Nova SMC 2016', Astrophysical Journal, vol. 862, no. 2, 164. https://doi.org/10.3847/1538-4357/aacf06
Orio M, Ness JU, Dobrotka A, Gatuzz E, Ospina N, Aydi E et al. What We Learn from the X-Ray Grating Spectra of Nova SMC 2016. Astrophysical Journal. 2018 Aug 1;862(2). 164. https://doi.org/10.3847/1538-4357/aacf06
Orio, M. ; Ness, J. U. ; Dobrotka, A. ; Gatuzz, E. ; Ospina, N. ; Aydi, E. ; Behar, E. ; Buckley, D. A.H. ; Ciroi, S. ; Della Valle, M. ; Hernanz, M. ; Henze, M. ; Osborne, J. P. ; Page, K. L. ; Rauch, T. ; Sala, G. ; Starrfield, Sumner ; Williams, R. E. ; Woodward, C. E. ; Zemko, P. / What We Learn from the X-Ray Grating Spectra of Nova SMC 2016. In: Astrophysical Journal. 2018 ; Vol. 862, No. 2.
@article{98cf5f6240af4ec8b34c4322a7f390e2,
title = "What We Learn from the X-Ray Grating Spectra of Nova SMC 2016",
abstract = "Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between days 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera, and the Low Energy Transmission Grating on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon, and sulfur on day 39, and oxygen, nitrogen, and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blueshifted, by about 1800 km s-1 on day 39 and up to 2100 km s-1 in the following observations. Spectral lines attributed to low-ionization potential transitions in the interstellar medium are also observed. Assuming the distance to the Small Magellanic Cloud, the bolometric luminosity exceeded the Eddington level for at least three months. A preliminary analysis with atmospheric models indicates an effective temperature of around 700,000 K on day 39, peaking at the later dates in the 850,000-900,000 K range, as expected for a ≃1.25 M o WD. We suggest a possible classification as an oxygen-neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show a large, aperiodic flux variability, which is not associated with spectral variability. We detected red noise, but did not find periodic or quasiperiodic modulations.",
keywords = "novae, cataclysmic variables, stars: abundances, stars: dwarf novae, stars: individual (N SMC 2016a), X-rays: stars",
author = "M. Orio and Ness, {J. U.} and A. Dobrotka and E. Gatuzz and N. Ospina and E. Aydi and E. Behar and Buckley, {D. A.H.} and S. Ciroi and {Della Valle}, M. and M. Hernanz and M. Henze and Osborne, {J. P.} and Page, {K. L.} and T. Rauch and G. Sala and Sumner Starrfield and Williams, {R. E.} and Woodward, {C. E.} and P. Zemko",
year = "2018",
month = "8",
day = "1",
doi = "10.3847/1538-4357/aacf06",
language = "English (US)",
volume = "862",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - What We Learn from the X-Ray Grating Spectra of Nova SMC 2016

AU - Orio, M.

AU - Ness, J. U.

AU - Dobrotka, A.

AU - Gatuzz, E.

AU - Ospina, N.

AU - Aydi, E.

AU - Behar, E.

AU - Buckley, D. A.H.

AU - Ciroi, S.

AU - Della Valle, M.

AU - Hernanz, M.

AU - Henze, M.

AU - Osborne, J. P.

AU - Page, K. L.

AU - Rauch, T.

AU - Sala, G.

AU - Starrfield, Sumner

AU - Williams, R. E.

AU - Woodward, C. E.

AU - Zemko, P.

PY - 2018/8/1

Y1 - 2018/8/1

N2 - Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between days 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera, and the Low Energy Transmission Grating on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon, and sulfur on day 39, and oxygen, nitrogen, and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blueshifted, by about 1800 km s-1 on day 39 and up to 2100 km s-1 in the following observations. Spectral lines attributed to low-ionization potential transitions in the interstellar medium are also observed. Assuming the distance to the Small Magellanic Cloud, the bolometric luminosity exceeded the Eddington level for at least three months. A preliminary analysis with atmospheric models indicates an effective temperature of around 700,000 K on day 39, peaking at the later dates in the 850,000-900,000 K range, as expected for a ≃1.25 M o WD. We suggest a possible classification as an oxygen-neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show a large, aperiodic flux variability, which is not associated with spectral variability. We detected red noise, but did not find periodic or quasiperiodic modulations.

AB - Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between days 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera, and the Low Energy Transmission Grating on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon, and sulfur on day 39, and oxygen, nitrogen, and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blueshifted, by about 1800 km s-1 on day 39 and up to 2100 km s-1 in the following observations. Spectral lines attributed to low-ionization potential transitions in the interstellar medium are also observed. Assuming the distance to the Small Magellanic Cloud, the bolometric luminosity exceeded the Eddington level for at least three months. A preliminary analysis with atmospheric models indicates an effective temperature of around 700,000 K on day 39, peaking at the later dates in the 850,000-900,000 K range, as expected for a ≃1.25 M o WD. We suggest a possible classification as an oxygen-neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show a large, aperiodic flux variability, which is not associated with spectral variability. We detected red noise, but did not find periodic or quasiperiodic modulations.

KW - novae, cataclysmic variables

KW - stars: abundances

KW - stars: dwarf novae

KW - stars: individual (N SMC 2016a)

KW - X-rays: stars

UR - http://www.scopus.com/inward/record.url?scp=85051492343&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85051492343&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/aacf06

DO - 10.3847/1538-4357/aacf06

M3 - Article

AN - SCOPUS:85051492343

VL - 862

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 164

ER -