VERY EARLY ULTRAVIOLET AND OPTICAL OBSERVATIONS OF THE TYPE Ia SUPERNOVA 2009ig

Foley, R. J.; Challis, Peter; Filippenko, A. V.; Ganeshalingam, M.; Landsman, W. B.; Li, W.; Marion, G. H.; Silverman, J. M.; Beaton, Rachael L.; Bennert, Vardha N.; Cenko, S. Bradley; Childress, M.; Guhathakurta, Puragra; Jiang, Linhua; Kalirai, Jason; Kirshner, R.; Stockton, Alan; Tollerud, Erik; Vinkó, J.; Wheeler, J. C.; Woo, Jong-Hak

doi:10.1088/0004-637x/744/1/38

Cited by 141 publications

(220 citation statements)

References 82 publications

(136 reference statements)

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“…Fitting a 4th order polynomial to the magnitudes obtained between +9 and +30 days after explosion resulted in t Bmax = JD 2 455 814.4 ± 0.6, which was used as input for the LC fitter codes (see below). Thus, the B-band maximum occured ∼17.2 days after explosion, very similar to the value derived by Foley et al (2012a) for SN 2009ig (17.13 days), which was also discovered in less than a day after explosion. The average value for the majority of "normal" SNe Ia is ∼17.4 ± 0.2 days (Hayden et al 2010).…”

Section: Constraining the Moment Of Explosion And B-band Maximumsupporting

confidence: 86%

“…The pre-maximum LC of SNe Ia can be surprisingly well described by the constant temperature "fireball" model (e.g. Arnett 1982;Nugent et al 2011;Foley et al 2012a). In this simple model the adiabatic loss of the ejecta internal energy is just compensated by the energy input from the radioactive decay of the 56 Ni and 56 Co synthesized during the explosion.…”

Section: Constraining the Moment Of Explosion And B-band Maximummentioning

confidence: 99%

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Testing supernovae Ia distance measurement methods with SN 2011fe

Vinkó¹,

Sárneczky²,

Takáts³

et al. 2012

A&A

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Aims. The nearby, bright, almost completely unreddened Type Ia supernova 2011fe in M101 provides a unique opportunity to test both the precision and the accuracy of the extragalactic distances derived from SNe Ia light curve fitters. Methods. We applied the current, public versions of the independent light curve fitting codes MLCS2k2 and SALT2 to compute the distance modulus of SN 2011fe from high-precision, multi-color (BVRI) light curves. Results. The results from the two fitting codes confirm that 2011fe is a "normal" (not peculiar) and only slightly reddened SN Ia. New unreddened distance moduli are derived as 29.21 ± 0.07 mag (D ∼ 6.95 ± 0.23 Mpc, MLCS2k2), and 29.05 ± 0.07 mag (6.46 ± 0.21 Mpc). Conclusions. Despite the very good fitting quality achieved with both light curve fitters, the resulting distance moduli are inconsistent by 2σ. Both are marginally consistent (at ∼1σ) with the Hubble Space Telescope key project distance modulus for M101. The SALT2 distance is in good agreement with the recently revised Cepheid-and TRGB-distance to M101. Averaging all SN-and Cepheid-based estimates, the absolute distance to M101 is ∼6.6 ± 0.5 Mpc.

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Section: Constraining the Moment Of Explosion And B-band Maximumsupporting

confidence: 86%

Section: Constraining the Moment Of Explosion And B-band Maximummentioning

confidence: 99%

Testing supernovae Ia distance measurement methods with SN 2011fe

Vinkó¹,

Sárneczky²,

Takáts³

et al. 2012

A&A

Self Cite

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“…Extremely nearby SNe Ia which were discovered soon after explosion have recently led to tight constraints on the size and luminosity of the companion star, thus ruling out many plausible SD scenarios for these objects (e.g., Nugent et al 2011;Ganeshalingam et al 2011;Brown et al 2012;Foley et al 2012a;Bloom et al 2012;Silverman et al 2012b). In addition, the so-called super-Chandrasekhar mass SNe Ia are thought to contain >1.4 M of SN ejecta and thus are likely formed from the DD scenario (e.g., Howell et al 2006;Yamanaka et al 2009;Scalzo et al 2010;Silverman et al 2011;Taubenberger et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Silverman¹,

Nugent

Gal‐Yam

et al. 2015

Proc. IAU

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Owing to their utility for measurements of cosmic acceleration, Type Ia supernovae (SNe Ia) are perhaps the beststudied class of SNe, yet the progenitor systems of these explosions largely remain a mystery. A rare subclass of SNe Ia shows evidence of strong interaction with their circumstellar medium (CSM), and in particular, a hydrogenrich CSM; we refer to them as SNe Ia-CSM. In the first systematic search for such systems, we have identified 16 SNe Ia-CSM, and here we present new spectra of 13 of them. Six SNe Ia-CSM have been well studied previously, three were previously known but are analyzed in depth for the first time here, and seven are new discoveries from the Palomar Transient Factory. The spectra of all SNe Ia-CSM are dominated by Hα emission (with widths of ∼2000 km s −1 ) and exhibit large Hα/Hβ intensity ratios (perhaps due to collisional excitation of hydrogen via the SN ejecta overtaking slower-moving CSM shells); moreover, they have an almost complete lack of He i emission. They also show possible evidence of dust formation through a decrease in the red wing of Hα 75-100 days past maximum brightness, and nearly all SNe Ia-CSM exhibit strong Na i D absorption from the host galaxy. The absolute magnitudes (uncorrected for host-galaxy extinction) of SNe Ia-CSM are found to be −21.3 mag M R −19 mag, and they also seem to show ultraviolet emission at early times and strong infrared emission at late times (but no detected radio or X-ray emission). Finally, the host galaxies of SNe Ia-CSM are all late-type spirals similar to the Milky Way, or dwarf irregulars like the Large Magellanic Cloud, which implies that these objects come from a relatively young stellar population. This work represents the most detailed analysis of the SN Ia-CSM class to date.

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“…To date ∼ 30 SNe Ia and ∼ 20 core collapse SNe have been targeted for grism observations. Despite the large number of targets, the number of published UVOT spectra of SNe remains quite small (Bufano et al 2009;Foley et al 2012;Bayless et al 2013;Brown et al 2014bBrown et al , 2015Margutti et al 2014). This is partly due to the fact that roughly half of the SNe Ia grism observations contain contamination which cannot be removed using the normal image processing methods and thus render the final spectral features and calibrations suspect or useless.…”

Section: Motivationmentioning

confidence: 99%

“…We calculated phases relative to B-band maximum light using the peak time of Foley et al (2012) occurring at JD = 2455080.5.…”

Section: Sn 2009igmentioning

confidence: 99%

DecontaminatingSwiftUVOT Grism Observations of Transient Sources

Smitka¹,

Brown²,

Kuin³

et al. 2016

PASP

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We present a new technique of decontaminating Swift UVOT grism spectra for transient objects. We describe the template image requirements and image processing steps necessary to successfully implement the empirical decontamination technique. We demonstrate the accuracy of the flux and wavelength calibrations for decontaminated spectra by comparing a spectrum of SN 2011fe with a well-calibrated, long-slit ultraviolet spectrum from the Hubble Space Telescope's Space Telescope Imaging Spectrograph. We also show how the decontamination removes spurious emission lines from spectra of iPTF14bdn which otherwise could be misinterpreted as coming from the supernova. The software which implements this technique is briefly discussed and is made available to the community.

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VERY EARLY ULTRAVIOLET AND OPTICAL OBSERVATIONS OF THE TYPE Ia SUPERNOVA 2009ig

Cited by 141 publications

References 82 publications

Testing supernovae Ia distance measurement methods with SN 2011fe

Testing supernovae Ia distance measurement methods with SN 2011fe

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

DecontaminatingSwiftUVOT Grism Observations of Transient Sources

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