ULTRAVIOLET LIGHT CURVES OF SUPERNOVAE WITH THE SWIFT ULTRAVIOLET/OPTICAL TELESCOPE

By P. Brown, S. Holland, S. Immler, P. Milne, P. Roming, N. Gehrels, J. Nousek, N. Panagia, M. Still, D. V. vanden Berk. 2009

142 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d2fe4a5691108e5e70f09fa8cc5b164d2d0b4f9c

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Citations in the corpus

• An Embedded X-Ray Source Shines through the Aspherical AT 2018cow: Revealing the Inner Workings of the Most Luminous Fast-evolving Optical Transients (2018, methodology): “We extracted aperture photometry following standard prescriptions by Brown et al. (2009), with the updated calibration files and revised zero points by Breeveld et al. (2011).”
• THE AFTERGLOW OF GRB 130427A FROM 1 TO 1016 GHz (2013, methodology): “We reduced the UVOT data using standard procedures within the HEASoft29 environment (e.g., Brown et al. 2009).”
• Type II-Plateau supernova radiation: dependences on progenitor and explosion properties (2013, background): “…Type II SN colors arising from compact BSG-star explosions (e.g., SN 1987A, for which CMFGEN does reproduce theU -band fading satisfactorily when the model atoms are complete enough; Dessart & Hillier 2010; Li et al. 2012) and from more extended RSG-star explosions (see, e.g., Brown et al. 2009).”
• OPTICAL DISCOVERY OF PROBABLE STELLAR TIDAL DISRUPTION FLARES (2010, background): “…assume that the UV flux falls off with the slowest linear decay rate of UV magnitude that has been measured for a large sample of Ia, Ib/c and type II SN (Brown et al. 2009): dmNUV/dt = 0.05magday −1, which is similar to the UV decay rate of SN 2008es (Gezari et al. 2009a; Miller et al. 2009).”
• A PANCHROMATIC VIEW OF THE RESTLESS SN 2009ip REVEALS THE EXPLOSIVE EJECTION OF A MASSIVE STAR ENVELOPE (2013, methodology): “Data have been analyzed following the prescriptions by Brown et al. (2009).”
• VARIABLE SODIUM ABSORPTION IN A LOW-EXTINCTION TYPE Ia SUPERNOVA, (2009, background): “…et al. 2008) to normalize the total number of UV–IR photons (1500−12000 Å) in the model spectrum.28 The model spectrum is only available for the time of maximum brightness, so we assume that the light curve at all UV wavelengths follows the SN 2007af UV W2 light curve from Brown et al. (2009).”
• Supernovae from red supergiants with extensive mass loss (2010, background): “For example, no Type IIP SNe observed with Swift satellite show the long term UV-brightening which is expected by CSM interaction (Brown et al. 2009).”
• PS16dtm: A Tidal Disruption Event in a Narrow-line Seyfert 1 Galaxy (2017, methodology): “We followed the prescriptions of Brown et al. (2009) with the updated calibration files and revised zero points of Breeveld et al. (2011).”
• The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models (2017, methodology): “We performed photometry in a 3 photometric aperture to in order minimize the contamination from host galaxy light, following the prescriptions by Brown et al. (2009).”
• The diversity of Type II supernova versus the similarity in their progenitors (2016, methodology): “Details about the pipeline can be found in Appendix B. Swift aperture photometry was computed following the prescriptions described by Brown et al. (2009), but using the updated zeropoints of Breeveld et al. (2010).”
• The first month of evolution of the slow-rising Type IIP SN 2013ej in M74 (2013, methodology): “…(for griz) or Landolt (1992) system (for UBVRI) via standard star observations taken during clear nights. on 2013 July 30.87 UT. Swift photometry, going from the uw2 filter through the V filter, has been measured using an aperture of 3 arcsec, and following the approach of Brown et al. (2009).”
• A NEW POPULATION OF ULTRA-LONG DURATION GAMMA-RAY BURSTS (2013, background): “In the former case the SNe would need to be relatively blue, perhaps akin to the early time (∼ 15 days) UV to optical spectrum of SNe II-P, such as SN 2005cs, or 2012aw35 (Pastorello et al. 2006; Brown et al. 2009; Bayless et al. 2012), although it would necessarily be much brighter with MV ∼ −18.5.”
• PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 (2016, methodology): “Photometry was obtained as described by Brown et al. (2009), and an aperture with radius 5′′ was used.”