Type IIb supernova SN 2011dh: Spectra and photometry from the ultraviolet to the near-infrared

G. H. Marion, Jozsef Vinko, Robert P. Kirshner, Ryan J. Foley, Perry Berlind, Allyson Bieryla, Joshua S. Bloom, Michael L. Calkins, Peter Challis, Roger A. Chevalier, Ryan Chornock, Chris Culliton, Jason L. Curtis, Gilbert A. Esquerdo, Mark E. Everett, Emilio E. Falco, Kevin France, Claes Fransson, Andrew S. Friedman, Peter GarnavichBruno Leibundgut, Samuel Meyer, Nathan Smith, Alicia M. Soderberg, Jesper Sollerman, Dan L. Starr, Tamas Szklenar, Katalin Takats, J. Craig Wheeler

Resultado de la investigación: Article

26 Citas (Scopus)

Resumen

We report spectroscopic and photometric observations of the Type IIb SN 2011dh obtained between 4 and 34 days after the estimated date of explosion (May 31.5 UT). The data cover a wide wavelength range from 2000 Å in the ultraviolet (UV) to 2.4 μm in the near-infrared (NIR). Optical spectra provide line profiles and velocity measurements of H I, He I, Ca II, and Fe II that trace the composition and kinematics of the supernova (SN). NIR spectra show that helium is present in the atmosphere as early as 11 days after the explosion. A UV spectrum obtained with the Space Telescope Imaging Spectrograph reveals that the UV flux for SN 2011dh is low compared to other SN IIb. Modeling the spectrum with SYNOW suggests that the UV deficit is due to line blanketing from Ti II and Co II. The H I and He I velocities in SN 2011dh are separated by about 4000 km s-1 at all phases. A velocity gap is consistent with models for a preexplosion structure in which a hydrogen-rich shell surrounds the progenitor. We estimate that the H shell of SN 2011dh is 8 times less massive than the shell of SN 1993J and3 times more massive than the shell of SN 2008ax. Light curves (LCs) for 12 passbands are presented: UVW2, UVM2, UVW1, U, u′, B, V, r′, i′, J, H, and Ks . In the B band, SN 2011dh reached peak brightness of 13.17 mag at 20.0 ± 0.5 after the explosion. The maximum bolometric luminosity of 1.8 ± 0.2 × 10 42 erg s-1 occurred22 days after the explosion. NIR emission provides more than 30% of the total bolometric flux at the beginning of our observations, and the NIR contribution increases to nearly 50% of the total by day 34. The UV produces 16% of the total flux on day 4, 5% on day 9, and 1% on day 34. We compare the bolometric LCs of SN 2011dh, SN 2008ax, and SN 1993J. The LC are very different for the first 12 days after the explosions, but all three SN IIb display similar peak luminosities, times of peak, decline rates, and colors after maximum. This suggests that the progenitors of these SN IIb may have had similar compositions and masses, but they exploded inside hydrogen shells that have a wide range of masses. SN 2011dh was well observed, and a likely progenitor star has been identified in preexplosion images. The detailed observations presented here will help evaluate theoretical models for this SN and lead to a better understanding of SN IIb.

Idioma originalEnglish
Número de artículo69
PublicaciónAstrophysical Journal
Volumen781
N.º2
DOI
EstadoPublished - 1 feb 2014

Huella dactilar

photometry
supernovae
explosion
near infrared
shell
hydrogen
explosions
erg
helium
light curve
kinematics
wavelength
atmosphere
modeling
luminosity
ultraviolet spectra
velocity measurement
spectrographs
optical spectrum
brightness

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Marion, G. H., Vinko, J., Kirshner, R. P., Foley, R. J., Berlind, P., Bieryla, A., ... Wheeler, J. C. (2014). Type IIb supernova SN 2011dh: Spectra and photometry from the ultraviolet to the near-infrared. Astrophysical Journal, 781(2), [69]. https://doi.org/10.1088/0004-637X/781/2/69
Marion, G. H. ; Vinko, Jozsef ; Kirshner, Robert P. ; Foley, Ryan J. ; Berlind, Perry ; Bieryla, Allyson ; Bloom, Joshua S. ; Calkins, Michael L. ; Challis, Peter ; Chevalier, Roger A. ; Chornock, Ryan ; Culliton, Chris ; Curtis, Jason L. ; Esquerdo, Gilbert A. ; Everett, Mark E. ; Falco, Emilio E. ; France, Kevin ; Fransson, Claes ; Friedman, Andrew S. ; Garnavich, Peter ; Leibundgut, Bruno ; Meyer, Samuel ; Smith, Nathan ; Soderberg, Alicia M. ; Sollerman, Jesper ; Starr, Dan L. ; Szklenar, Tamas ; Takats, Katalin ; Wheeler, J. Craig. / Type IIb supernova SN 2011dh : Spectra and photometry from the ultraviolet to the near-infrared. En: Astrophysical Journal. 2014 ; Vol. 781, N.º 2.
@article{b099f9c0e21b407bbcc694583962c4bc,
title = "Type IIb supernova SN 2011dh: Spectra and photometry from the ultraviolet to the near-infrared",
abstract = "We report spectroscopic and photometric observations of the Type IIb SN 2011dh obtained between 4 and 34 days after the estimated date of explosion (May 31.5 UT). The data cover a wide wavelength range from 2000 {\AA} in the ultraviolet (UV) to 2.4 μm in the near-infrared (NIR). Optical spectra provide line profiles and velocity measurements of H I, He I, Ca II, and Fe II that trace the composition and kinematics of the supernova (SN). NIR spectra show that helium is present in the atmosphere as early as 11 days after the explosion. A UV spectrum obtained with the Space Telescope Imaging Spectrograph reveals that the UV flux for SN 2011dh is low compared to other SN IIb. Modeling the spectrum with SYNOW suggests that the UV deficit is due to line blanketing from Ti II and Co II. The H I and He I velocities in SN 2011dh are separated by about 4000 km s-1 at all phases. A velocity gap is consistent with models for a preexplosion structure in which a hydrogen-rich shell surrounds the progenitor. We estimate that the H shell of SN 2011dh is 8 times less massive than the shell of SN 1993J and3 times more massive than the shell of SN 2008ax. Light curves (LCs) for 12 passbands are presented: UVW2, UVM2, UVW1, U, u′, B, V, r′, i′, J, H, and Ks . In the B band, SN 2011dh reached peak brightness of 13.17 mag at 20.0 ± 0.5 after the explosion. The maximum bolometric luminosity of 1.8 ± 0.2 × 10 42 erg s-1 occurred22 days after the explosion. NIR emission provides more than 30{\%} of the total bolometric flux at the beginning of our observations, and the NIR contribution increases to nearly 50{\%} of the total by day 34. The UV produces 16{\%} of the total flux on day 4, 5{\%} on day 9, and 1{\%} on day 34. We compare the bolometric LCs of SN 2011dh, SN 2008ax, and SN 1993J. The LC are very different for the first 12 days after the explosions, but all three SN IIb display similar peak luminosities, times of peak, decline rates, and colors after maximum. This suggests that the progenitors of these SN IIb may have had similar compositions and masses, but they exploded inside hydrogen shells that have a wide range of masses. SN 2011dh was well observed, and a likely progenitor star has been identified in preexplosion images. The detailed observations presented here will help evaluate theoretical models for this SN and lead to a better understanding of SN IIb.",
keywords = "infrared: general, supernovae: general, supernovae: individual (2011dh), ultraviolet: general",
author = "Marion, {G. H.} and Jozsef Vinko and Kirshner, {Robert P.} and Foley, {Ryan J.} and Perry Berlind and Allyson Bieryla and Bloom, {Joshua S.} and Calkins, {Michael L.} and Peter Challis and Chevalier, {Roger A.} and Ryan Chornock and Chris Culliton and Curtis, {Jason L.} and Esquerdo, {Gilbert A.} and Everett, {Mark E.} and Falco, {Emilio E.} and Kevin France and Claes Fransson and Friedman, {Andrew S.} and Peter Garnavich and Bruno Leibundgut and Samuel Meyer and Nathan Smith and Soderberg, {Alicia M.} and Jesper Sollerman and Starr, {Dan L.} and Tamas Szklenar and Katalin Takats and Wheeler, {J. Craig}",
year = "2014",
month = "2",
day = "1",
doi = "10.1088/0004-637X/781/2/69",
language = "English",
volume = "781",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

Marion, GH, Vinko, J, Kirshner, RP, Foley, RJ, Berlind, P, Bieryla, A, Bloom, JS, Calkins, ML, Challis, P, Chevalier, RA, Chornock, R, Culliton, C, Curtis, JL, Esquerdo, GA, Everett, ME, Falco, EE, France, K, Fransson, C, Friedman, AS, Garnavich, P, Leibundgut, B, Meyer, S, Smith, N, Soderberg, AM, Sollerman, J, Starr, DL, Szklenar, T, Takats, K & Wheeler, JC 2014, 'Type IIb supernova SN 2011dh: Spectra and photometry from the ultraviolet to the near-infrared', Astrophysical Journal, vol. 781, n.º 2, 69. https://doi.org/10.1088/0004-637X/781/2/69

Type IIb supernova SN 2011dh : Spectra and photometry from the ultraviolet to the near-infrared. / Marion, G. H.; Vinko, Jozsef; Kirshner, Robert P.; Foley, Ryan J.; Berlind, Perry; Bieryla, Allyson; Bloom, Joshua S.; Calkins, Michael L.; Challis, Peter; Chevalier, Roger A.; Chornock, Ryan; Culliton, Chris; Curtis, Jason L.; Esquerdo, Gilbert A.; Everett, Mark E.; Falco, Emilio E.; France, Kevin; Fransson, Claes; Friedman, Andrew S.; Garnavich, Peter; Leibundgut, Bruno; Meyer, Samuel; Smith, Nathan; Soderberg, Alicia M.; Sollerman, Jesper; Starr, Dan L.; Szklenar, Tamas; Takats, Katalin; Wheeler, J. Craig.

En: Astrophysical Journal, Vol. 781, N.º 2, 69, 01.02.2014.

Resultado de la investigación: Article

TY - JOUR

T1 - Type IIb supernova SN 2011dh

T2 - Spectra and photometry from the ultraviolet to the near-infrared

AU - Marion, G. H.

AU - Vinko, Jozsef

AU - Kirshner, Robert P.

AU - Foley, Ryan J.

AU - Berlind, Perry

AU - Bieryla, Allyson

AU - Bloom, Joshua S.

AU - Calkins, Michael L.

AU - Challis, Peter

AU - Chevalier, Roger A.

AU - Chornock, Ryan

AU - Culliton, Chris

AU - Curtis, Jason L.

AU - Esquerdo, Gilbert A.

AU - Everett, Mark E.

AU - Falco, Emilio E.

AU - France, Kevin

AU - Fransson, Claes

AU - Friedman, Andrew S.

AU - Garnavich, Peter

AU - Leibundgut, Bruno

AU - Meyer, Samuel

AU - Smith, Nathan

AU - Soderberg, Alicia M.

AU - Sollerman, Jesper

AU - Starr, Dan L.

AU - Szklenar, Tamas

AU - Takats, Katalin

AU - Wheeler, J. Craig

PY - 2014/2/1

Y1 - 2014/2/1

N2 - We report spectroscopic and photometric observations of the Type IIb SN 2011dh obtained between 4 and 34 days after the estimated date of explosion (May 31.5 UT). The data cover a wide wavelength range from 2000 Å in the ultraviolet (UV) to 2.4 μm in the near-infrared (NIR). Optical spectra provide line profiles and velocity measurements of H I, He I, Ca II, and Fe II that trace the composition and kinematics of the supernova (SN). NIR spectra show that helium is present in the atmosphere as early as 11 days after the explosion. A UV spectrum obtained with the Space Telescope Imaging Spectrograph reveals that the UV flux for SN 2011dh is low compared to other SN IIb. Modeling the spectrum with SYNOW suggests that the UV deficit is due to line blanketing from Ti II and Co II. The H I and He I velocities in SN 2011dh are separated by about 4000 km s-1 at all phases. A velocity gap is consistent with models for a preexplosion structure in which a hydrogen-rich shell surrounds the progenitor. We estimate that the H shell of SN 2011dh is 8 times less massive than the shell of SN 1993J and3 times more massive than the shell of SN 2008ax. Light curves (LCs) for 12 passbands are presented: UVW2, UVM2, UVW1, U, u′, B, V, r′, i′, J, H, and Ks . In the B band, SN 2011dh reached peak brightness of 13.17 mag at 20.0 ± 0.5 after the explosion. The maximum bolometric luminosity of 1.8 ± 0.2 × 10 42 erg s-1 occurred22 days after the explosion. NIR emission provides more than 30% of the total bolometric flux at the beginning of our observations, and the NIR contribution increases to nearly 50% of the total by day 34. The UV produces 16% of the total flux on day 4, 5% on day 9, and 1% on day 34. We compare the bolometric LCs of SN 2011dh, SN 2008ax, and SN 1993J. The LC are very different for the first 12 days after the explosions, but all three SN IIb display similar peak luminosities, times of peak, decline rates, and colors after maximum. This suggests that the progenitors of these SN IIb may have had similar compositions and masses, but they exploded inside hydrogen shells that have a wide range of masses. SN 2011dh was well observed, and a likely progenitor star has been identified in preexplosion images. The detailed observations presented here will help evaluate theoretical models for this SN and lead to a better understanding of SN IIb.

AB - We report spectroscopic and photometric observations of the Type IIb SN 2011dh obtained between 4 and 34 days after the estimated date of explosion (May 31.5 UT). The data cover a wide wavelength range from 2000 Å in the ultraviolet (UV) to 2.4 μm in the near-infrared (NIR). Optical spectra provide line profiles and velocity measurements of H I, He I, Ca II, and Fe II that trace the composition and kinematics of the supernova (SN). NIR spectra show that helium is present in the atmosphere as early as 11 days after the explosion. A UV spectrum obtained with the Space Telescope Imaging Spectrograph reveals that the UV flux for SN 2011dh is low compared to other SN IIb. Modeling the spectrum with SYNOW suggests that the UV deficit is due to line blanketing from Ti II and Co II. The H I and He I velocities in SN 2011dh are separated by about 4000 km s-1 at all phases. A velocity gap is consistent with models for a preexplosion structure in which a hydrogen-rich shell surrounds the progenitor. We estimate that the H shell of SN 2011dh is 8 times less massive than the shell of SN 1993J and3 times more massive than the shell of SN 2008ax. Light curves (LCs) for 12 passbands are presented: UVW2, UVM2, UVW1, U, u′, B, V, r′, i′, J, H, and Ks . In the B band, SN 2011dh reached peak brightness of 13.17 mag at 20.0 ± 0.5 after the explosion. The maximum bolometric luminosity of 1.8 ± 0.2 × 10 42 erg s-1 occurred22 days after the explosion. NIR emission provides more than 30% of the total bolometric flux at the beginning of our observations, and the NIR contribution increases to nearly 50% of the total by day 34. The UV produces 16% of the total flux on day 4, 5% on day 9, and 1% on day 34. We compare the bolometric LCs of SN 2011dh, SN 2008ax, and SN 1993J. The LC are very different for the first 12 days after the explosions, but all three SN IIb display similar peak luminosities, times of peak, decline rates, and colors after maximum. This suggests that the progenitors of these SN IIb may have had similar compositions and masses, but they exploded inside hydrogen shells that have a wide range of masses. SN 2011dh was well observed, and a likely progenitor star has been identified in preexplosion images. The detailed observations presented here will help evaluate theoretical models for this SN and lead to a better understanding of SN IIb.

KW - infrared: general

KW - supernovae: general

KW - supernovae: individual (2011dh)

KW - ultraviolet: general

UR - http://www.scopus.com/inward/record.url?scp=84892772856&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/781/2/69

DO - 10.1088/0004-637X/781/2/69

M3 - Article

AN - SCOPUS:84892772856

VL - 781

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 69

ER -