UBVRI photometry of SN 1993J in M81: The first 120 days

Richmond, M.; Treffers, R. R.; Filippenko, A. V.; Paik, Young; Leibundgut, B.; Schulman, Eric; Cox, Caroline V.

doi:10.1086/116915

Cited by 231 publications

(245 citation statements)

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“…This contrasts with previous early UV observations of Type II SNe, i.e., the Type II-pec SN 1987A (Hamuy et al 1988), the Type IIb SN 1993J (Schmidt et al 1993;Richmond et al 1994), and the Type II-P SN 2006bp (Immler et al 2007;Dessart et al 2008, hereafter D08), in which they were all fading in the UV, since the SN ejecta had already begun their long-term cooling phase through expansion and radiation. In § 2, we describe the GALEX and SNLS observations.…”

Section: Introductioncontrasting

confidence: 70%

Probing Shock Breakout with Serendipitous GALEX Detections of Two SNLS Type II-P Supernovae

Gezari

Dessart

Basa

et al. 2008

ApJ

112

145

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We report the serendipitous detection by GALEX of fast (!1 day) rising (տ1 mag) UV emission from two Type II plateau (II-P) supernovae (SNe) at and 0.324 discovered by the Supernova Legacy Survey. Optical z p 0.185 photometry and VLT spectroscopy 2 weeks after the GALEX detections link the onset of UV emission to the time of shock breakout. Using radiation hydrodynamics and non-LTE radiative transfer simulations, and starting from a standard red supergiant (RSG; Type II-P SN progenitor) star evolved self-consistently from the main sequence to iron core collapse, we model the shock breakout phase and the 55 hr that follow. The small scale height of our RSG atmosphere model suggests that the breakout signature is a thermal soft X-ray burst ( ) with å l ∼ 90 A peak duration of Շ2000 s. Longer durations are possible but require either an extended and tenuous nonstandard envelope or an unusually dense RSG wind with yr Ϫ1 . The GALEX observations miss the peak of the luminous) UV burst but unambiguously capture the rise of the emission and a subsequent 2 day long plateau. M ≈ Ϫ20 FUVThe postbreakout, UV-bright plateau is a prediction of our model in which the shift of the peak of the spectral energy distribution (SED) from ∼100 to ∼1000 and the ejecta expansion both counteract the decrease in bolometric A luminosity from ∼10 11 to ∼10 9 over that period. Based on the observed detection efficiency of our study, we L , make predictions for the breakout detection rate of the GALEX Time Domain Survey.

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Section: Introductioncontrasting

confidence: 70%

Probing Shock Breakout with Serendipitous GALEX Detections of Two SNLS Type II-P Supernovae

Gezari

Dessart

Basa

et al. 2008

ApJ

112

145

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“…The derived extinction is much higher than toward SN 1993J, for which Richmond et al (1994) discuss values of A V = 0.7 and 1.0 mag. With the extinction law given by Cardelli et al (1989), A K = 0.114 A V , we calculate 2.8 mag for the K-band (2.2 μm) extinction.…”

Section: Column Density and Extinctionmentioning

confidence: 71%

VLBI observations of SN 2008iz

Brunthaler¹,

Martí-Vidal²,

Menten³

et al. 2010

A&A

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We present observations of the recently discovered supernova 2008iz in M 82 with the VLBI High Sensitivity Array at 22 GHz, the Very Large Array at frequencies of 1. 4, 4.8, 8.4, 22 and 43 GHz, and the Chandra X-ray observatory. The supernova was clearly detected in two VLBI images separated by 11 months. The source shows a ring-like morphology and expands with a velocity of ∼23 000 km s −1 . The most likely explosion date is in mid-February 2008. The measured expansion speed is a factor of ∼2 higher than expected under the assumption that synchrotron self-absorption dominates the light curve at the peak, indicating that this absorption mechanism may not be important for the radio emission. We find no evidence for an asymmetric explosion. The VLA spectrum shows a broken power law, indicating that the source was still optically thick at 1.4 GHz in April 2009. Finally, we report upper limits on the X-ray emission from SN 2008iz and a second radio transient recently discovered by MERLIN observations.

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“…The extinction within the Milky Way as given by the S98 extinction maps recalibrated by SF11 is E(B − V) MW = 0.07 mag. Richmond et al (1994) discuss the extinction in some detail and suggest a total E(B − V) T between 0.08 and 0.32 mag. High-resolution spectroscopy of the Na  D lines was presented in Bowen et al (1994).…”

Section: Sn 1993jmentioning

confidence: 92%

Optical and near-infrared observations of SN 2011dh – The first 100 days

Ergon

Sollerman

Fraser

et al. 2014

A&A

111

125

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We present optical and near-infrared (NIR) photometry and spectroscopy of the Type IIb supernova (SN) 2011dh for the first 100 days. We complement our extensive dataset with Swift ultra-violet (UV) and Spitzer mid-infrared (MIR) data to build a UV to MIR bolometric lightcurve using both photometric and spectroscopic data. Hydrodynamical modelling of the SN based on this bolometric lightcurve have been presented in Bersten et al. (2012, ApJ, 757, 31). We find that the absorption minimum for the hydrogen lines is never seen below ∼11 000 km s −1 but approaches this value as the lines get weaker. This suggests that the interface between the helium core and hydrogen rich envelope is located near this velocity in agreement with the Bersten et al. (2012) He4R270 ejecta model. Spectral modelling of the hydrogen lines using this ejecta model supports the conclusion and we find a hydrogen mass of 0.01-0.04 M to be consistent with the observed spectral evolution. We estimate that the photosphere reaches the helium core at 5-7 days whereas the helium lines appear between ∼10 and ∼15 days, close to the photosphere and then move outward in velocity until ∼40 days. This suggests that increasing non-thermal excitation due to decreasing optical depth for the γ-rays is driving the early evolution of these lines. The Spitzer 4.5 µm band shows a significant flux excess, which we attribute to CO fundamental band emission or a thermal dust echo although further work using late time data is needed. The distance and in particular the extinction, where we use spectral modelling to put further constraints, is discussed in some detail as well as the sensitivity of the hydrodynamical modelling to errors in these quantities. We also provide and discuss pre-and post-explosion observations of the SN site which shows a reduction by ∼75 percent in flux at the position of the yellow supergiant coincident with SN 2011dh. The B, V and r band decline rates of 0.0073, 0.0090 and 0.0053 mag day −1 respectively are consistent with the remaining flux being emitted by the SN. Hence we find that the star was indeed the progenitor of SN 2011dh as previously suggested by Maund et al. (2011, ApJ, 739, L37) and which is also consistent with the results from the hydrodynamical modelling.

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UBVRI photometry of SN 1993J in M81: The first 120 days

Cited by 231 publications

References 0 publications

Probing Shock Breakout with Serendipitous GALEX Detections of Two SNLS Type II-P Supernovae

Probing Shock Breakout with Serendipitous GALEX Detections of Two SNLS Type II-P Supernovae

VLBI observations of SN 2008iz

Optical and near-infrared observations of SN 2011dh – The first 100 days

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