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Title: The detection rate of early UV emission from supernovae: A dedicated GALEX/PTF survey and calibrated theoretical estimates

Abstract

The radius and surface composition of an exploding massive star, as well as the explosion energy per unit mass, can be measured using early UV observations of core-collapse supernovae (SNe). We present the first results from a simultaneous GALEX/PTF search for early ultraviolet (UV) emission from SNe. Six SNe II and one Type II superluminous SN (SLSN-II) are clearly detected in the GALEX near-UV (NUV) data. We compare our detection rate with theoretical estimates based on early, shock-cooling UV light curves calculated from models that fit existing Swift and GALEXobservations well, combined with volumetric SN rates. We find that our observations are in good agreement with calculated rates assuming that red supergiants (RSGs) explode with fiducial radii of 500 R⊙, explosion energies of 1051 erg, and ejecta masses of 10 M⊙. Exploding blue supergiants and Wolf-Rayet stars are poorly constrained. We describe how such observations can be used to derive the progenitor radius, surface composition, and explosion energy per unit mass of such SN events, and we demonstrate why UV observations are critical for such measurements. We use the fiducial RSG parameters to estimate the detection rate of SNe during the shock-cooling phase (<1 day after explosion) for several ground-basedmore » surveys (PTF, ZTF, and LSST). We show that the proposed wide-field UV explorer ULTRASAT mission is expected to find >85 SNe per year (~0.5 SN per deg2), independent of host galaxy extinction, down to an NUV detection limit of 21.5 mag AB. Lastly, our pilot GALEX/PTF project thus convincingly demonstrates that a dedicated, systematic SN survey at the NUV band is a compelling method to study how massive stars end their life.« less

Authors:
 [1];  [1];  [1];  [1];  [1];  [1];  [2];  [3];  [2];  [4];  [4];  [5];  [5];  [6];  [6];  [6];  [7];  [2];  [2];  [2] more »;  [2];  [8];  [9];  [10];  [11] « less
+ Show Author Affiliations
  1. The Weizmann Institute of Science, Rehovot (Israel)
  2. California Inst. of Technology (CalTech), Pasadena, CA (United States)
  3. Harvard-Smithsonian Ctr. for Astrophysics, Cambridge, MA (United States)
  4. Univ. of Haifa, Haifa (Israel)
  5. Technion Israel Institute of Technology, Haifa (Israel)
  6. Tel Aviv Univ., Tel Aviv (Israel)
  7. ETH Zurich, Zurich (Switzerland)
  8. Las Cumbres Observatory Global Telescope, Goleta, CA (United States); Univ. of California, Santa Barbara, CA (United States)
  9. Univ. of California, Berkeley, CA (United States)
  10. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  11. Univ. of Southampton, Southampton (United Kingdom)
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
Contributing Org.:
The ULTRASAT Science Team; The WTTH consortium; the GALEX Science Team; The Palomar Transient Factory
OSTI Identifier:
1525138
Grant/Contract Number:  
AC02-05CH11231
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 820; Journal Issue: 1; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; supernovae: general

Citation Formats

Ganot, Noam, Gal-Yam, Avishay, Ofek, Eran. O., Sagiv, Ilan, Waxman, Eli, Lapid, Ofer, Kulkarni, Shrinivas R., Ben-Ami, Sagi, Kasliwal, Mansi M., Chelouche, Doron, Rafter, Stephen, Behar, Ehud, Laor, Ari, Poznanski, Dovi, Nakar, Ehud, Maoz, Dan, Trakhtenbrot, Benny, Neill, James D., Barlow, Thomas A., Martin, Christofer D., Gezari, Suvi, Arcavi, Iair, Bloom, Joshua S., Nugent, Peter E., and Sullivan, Mark. The detection rate of early UV emission from supernovae: A dedicated GALEX/PTF survey and calibrated theoretical estimates. United States: N. p., 2016. Web. doi:10.3847/0004-637X/820/1/57.
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Ganot, Noam, Gal-Yam, Avishay, Ofek, Eran. O., Sagiv, Ilan, Waxman, Eli, Lapid, Ofer, Kulkarni, Shrinivas R., Ben-Ami, Sagi, Kasliwal, Mansi M., Chelouche, Doron, Rafter, Stephen, Behar, Ehud, Laor, Ari, Poznanski, Dovi, Nakar, Ehud, Maoz, Dan, Trakhtenbrot, Benny, Neill, James D., Barlow, Thomas A., Martin, Christofer D., Gezari, Suvi, Arcavi, Iair, Bloom, Joshua S., Nugent, Peter E., & Sullivan, Mark. The detection rate of early UV emission from supernovae: A dedicated GALEX/PTF survey and calibrated theoretical estimates. United States. https://doi.org/10.3847/0004-637X/820/1/57
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Ganot, Noam, Gal-Yam, Avishay, Ofek, Eran. O., Sagiv, Ilan, Waxman, Eli, Lapid, Ofer, Kulkarni, Shrinivas R., Ben-Ami, Sagi, Kasliwal, Mansi M., Chelouche, Doron, Rafter, Stephen, Behar, Ehud, Laor, Ari, Poznanski, Dovi, Nakar, Ehud, Maoz, Dan, Trakhtenbrot, Benny, Neill, James D., Barlow, Thomas A., Martin, Christofer D., Gezari, Suvi, Arcavi, Iair, Bloom, Joshua S., Nugent, Peter E., and Sullivan, Mark. Thu . "The detection rate of early UV emission from supernovae: A dedicated GALEX/PTF survey and calibrated theoretical estimates". United States. https://doi.org/10.3847/0004-637X/820/1/57. https://www.osti.gov/servlets/purl/1525138.
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@article{osti_1525138,
title = {The detection rate of early UV emission from supernovae: A dedicated GALEX/PTF survey and calibrated theoretical estimates},
author = {Ganot, Noam and Gal-Yam, Avishay and Ofek, Eran. O. and Sagiv, Ilan and Waxman, Eli and Lapid, Ofer and Kulkarni, Shrinivas R. and Ben-Ami, Sagi and Kasliwal, Mansi M. and Chelouche, Doron and Rafter, Stephen and Behar, Ehud and Laor, Ari and Poznanski, Dovi and Nakar, Ehud and Maoz, Dan and Trakhtenbrot, Benny and Neill, James D. and Barlow, Thomas A. and Martin, Christofer D. and Gezari, Suvi and Arcavi, Iair and Bloom, Joshua S. and Nugent, Peter E. and Sullivan, Mark},
abstractNote = {The radius and surface composition of an exploding massive star, as well as the explosion energy per unit mass, can be measured using early UV observations of core-collapse supernovae (SNe). We present the first results from a simultaneous GALEX/PTF search for early ultraviolet (UV) emission from SNe. Six SNe II and one Type II superluminous SN (SLSN-II) are clearly detected in the GALEX near-UV (NUV) data. We compare our detection rate with theoretical estimates based on early, shock-cooling UV light curves calculated from models that fit existing Swift and GALEXobservations well, combined with volumetric SN rates. We find that our observations are in good agreement with calculated rates assuming that red supergiants (RSGs) explode with fiducial radii of 500 R⊙, explosion energies of 1051 erg, and ejecta masses of 10 M⊙. Exploding blue supergiants and Wolf-Rayet stars are poorly constrained. We describe how such observations can be used to derive the progenitor radius, surface composition, and explosion energy per unit mass of such SN events, and we demonstrate why UV observations are critical for such measurements. We use the fiducial RSG parameters to estimate the detection rate of SNe during the shock-cooling phase (<1 day after explosion) for several ground-based surveys (PTF, ZTF, and LSST). We show that the proposed wide-field UV explorer ULTRASAT mission is expected to find >85 SNe per year (~0.5 SN per deg2), independent of host galaxy extinction, down to an NUV detection limit of 21.5 mag AB. Lastly, our pilot GALEX/PTF project thus convincingly demonstrates that a dedicated, systematic SN survey at the NUV band is a compelling method to study how massive stars end their life.},
doi = {10.3847/0004-637X/820/1/57},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 820,
place = {United States},
year = {Thu Mar 17 00:00:00 EDT 2016},
month = {Thu Mar 17 00:00:00 EDT 2016}
}
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Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record
https://doi.org/10.3847/0004-637X/820/1/57
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Cited by: 22 works
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Figures / Tables:

Fig. 1 Fig. 1: SN early UV emission models compared to data. At early times (< 3 hr post explosion) no optical/UV data exist. The models of Sapir et al. (2013; solid) and Nakar & Sari (2010; rescaled, see text; dashed) approximately agree in peak value, but differ in details. Forthcoming UVmore » surveys (e.g., ULTRASAT; Sagiv et al. 2014) will observe such early emission and further constrain models. At later times Rabinak & Waxman 2011 (RW11; solid) models for red supergiant stars (RSG; thick black) and compact W-R stars (He, thick cyan and C/O, thin cyan) compare well with UV observations from Swift/UVOT (SN 2008D, Type Ib, Soderberg et al. 2008; black solid circles) and GALEX/NUV (SNLS-04D2dc, Type II, Schawinski et al. 2008, Gezari et al. 2008, red solid circles). Blue supergiant (BSG) models (thin blue) are currently untested. Stellar classes (RSG/BSG/WR) differ greatly in their UV peaks making early UV observations a strong discriminator among progenitor classes. Plotted models assume reasonable parameters: RSG with R∗ = 500R⊙, explosion energy E= 2×1051 erg and ejected mass M= 10M⊙, BSG with R∗ = 50R⊙, E= 10 51 erg and identical mass, and a W-R star with either He or C/O dominated composition, R∗ = 1.15R⊙, E= 0.8 × 1051 erg and ejected mass M= 7.5M⊙. RW11 models are unextinguished, data points have been extinction corrected (by ANUV = 1.45 mag and ANUV = 2.2 mag for SNLS-04D2dc and SN 2008D, respectively) using the extinction values provided by Schawinsky et al. (2008) and RW11 (for SN 2008D).« less
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      Fig. 7 (p. 19)figure
      Fig. 88 (p. 20)figure
      Table 1 (p. 21)table
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      Table 2 (p. 28)table
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