CfA3: 185 TYPE Ia SUPERNOVA LIGHT CURVES FROM THE CfA

By M. Hicken, P. Challis, S. Jha, R. Kirshner, Thomas Matheson, Maryam Modjaz, Armin Rest, W. Michael Wood-Vasey, Gáspár Á. Bakos, E. Barton and 67 more. 2009

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We present multiband photometry of 185 type-Ia supernovae (SNe Ia), with over 11,500 observations. These were acquired between 2001 and 2008 at the F. L. Whipple Observatory of the Harvard-Smithsonian Center for Astrophysics (CfA). This sample contains the largest number of homogeneously observed and reduced nearby SNe Ia (z ≲ 0.08) published to date. It more than doubles the nearby sample, bringing SN Ia cosmology to the point where systematic uncertainties dominate. Our natural system photometry has a precision of ≲0.02 mag in BVRIr′i′ and ≲0.04 mag in U for points brighter than 17.5 mag. We also estimate a systematic uncertainty of 0.03 mag in our SN Ia standard system BVRIr′i′ photometry and 0.07 mag for U. Comparisons of our standard system photometry with published SN Ia light curves and comparison stars, where available for the same SN, reveal agreement at the level of a few hundredths mag in most cases. We find that 1991bg-like SNe Ia are sufficiently distinct from other SNe Ia in their color and light-curve-shape/luminosity relation that they should be treated separately in light-curve/distance fitter training samples. The CfA3 sample will contribute to the development of better light-curve/distance fitters, particularly in the few dozen cases where near-infrared photometry has been obtained and, together, can help disentangle host-galaxy reddening from intrinsic supernova color, reducing the systematic uncertainty in SN Ia distances due to dust.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/83c2d6ea821e11f17ef38f517d02caa1f04758ce

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Citations in the corpus

DOUBLE-DETONATION SUB-CHANDRASEKHAR SUPERNOVAE: SYNTHETIC OBSERVABLES FOR MINIMUM HELIUM SHELL MASS MODELS (2010, background): “Observationally, brighter SNe Ia show a trend of slower declining light curves (e.g., Phillips 1993; Hicken et al. 2009).”
Berkeley Supernova Ia Program – I. Observations, data reduction and spectroscopic sample of 582 low-redshift Type Ia supernovae (2012, methodology): “Many spectra presented in this paper have complementary light curves from Hamuy et al. (1996), Riess et al. (1999), Jha et al. (2006), Hicken et al. (2009), and Ganeshalingam et al. (2010), which have all been compiled and fit by Ganeshalingam et al. (in prep.).”
CfA4: LIGHT CURVES FOR 94 TYPE Ia SUPERNOVAE (2012, methodology): “At the Harvard-Smithsonian Center for Astrophysics (CfA), we have been engaged in building up the local sample, with 22 SN Ia light curves in the CfA1 sample (Riess et al. 1999), 44 in CfA2 (Jha et al. 2006), and 185 in CfA3 (Hicken et al. 2009a, hereafter H09).”
Observational probes of cosmic acceleration (2012, methodology): “Recent examples include the “Gold” sample (Riess et al., 2004, 2007), the “Union” and “Union2” samples (Kowalski et al., 2008; Amanullah et al., 2010), the “Constitution” sample (Hicken et al., 2009a), and the compilation of local, SDSS-II, SNLS3, and HST supernovae analyzed by Conley et al. (2011).”
A 2.4% DETERMINATION OF THE LOCAL VALUE OF THE HUBBLE CONSTANT (2016, methodology): “As in R11, we make use of several studies (Hicken et al. 2009b; Kelly et al. 2010; Lampeitl et al. 2010; Sullivan et al. 2010) which have shown the existence of a small step brighter for the corrected SN magnitude for hosts more massive than ~Mlog 10stellar .”
Measuring Dark Energy Properties with Photometrically Classified Pan-STARRS Supernovae. II. Cosmological Parameters (2017, methodology): “…Alam et al. 2015), the SuperNova Legacy Survey (SNLS; Astier et al. 2006) high-z SNe from HST (Riess et al. 2007) and low-z SNe (Hamuy et al. 1996; Riess et al. 1999; Jha et al. 2006; Hicken et al. 2009c,b; Contreras et al. 2010; Folatelli et al. 2010) to form the Joint Lightcurve Analysis (JLA).”
The WiggleZ Dark Energy Survey: mapping the distance-redshift relation with baryon acoustic oscillations (2011, methodology): “These projects include the Nearby Supernova Factory (Copin et al. 2006), the Center for Astrophysics SN group (Hicken et al. 2009), the Carnegie Supernova Project (Hamuy et al. 2006) and the Palomar Transient Factory (Law et al. 2009) at low redshifts z < 0.1; the Sloan Digital Sky Survey (SDSS)…”
The WiggleZ Dark Energy Survey: measuring the cosmic expansion history using the Alcock-Paczynski test and distant supernovae (2011, methodology): “This compilation of 557 supernovae includes data from Hamuy et al. (1996), Riess et al. (1999, 2007), Astier et al. (2006), Jha et al. (2006), Wood-Vasey et al. (2007), Holtzman et al. (2008), Hicken et al. (2009) and Kessler et al. (2009).”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “…et al. 2009; Reichardt et al. 2009; Brown et al. 2009), large-scale structure data (Reid et al. 2010a; Percival et al. 2009), supernova data (Hicken et al. 2009b; Kessler et al. 2009), cluster measurements (Vikhlinin et al. 2009b; Mantz et al. 2010c), distance measurements (Riess et al.…”
THE CARNEGIE SUPERNOVA PROJECT: FIRST PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE (2009, background): “Subsequently, this group has published UBV RI light curves of 44 events (Jha et al. 2006), and UBV RIr′i′ light curves of another 185 (Hicken et al. 2009).”
High luminosity, slow ejecta and persistent carbon lines: SN 2009dc challenges thermonuclear explosion scenarios (2010, background): “It is clearly brighter than all other SNe Ia (from the CfA3 data set; Hicken et al. 2009), and also ∼0.65 mag brighter than anticipated by the Phillips et al. (1999) relation for its m15(B) of 0.69.”
SPECTRA AND HUBBLE SPACE TELESCOPE LIGHT CURVES OF SIX TYPE Ia SUPERNOVAE AT 0.511 < z < 1.12 AND THE UNION2 COMPILATION (2010, methodology): “…Automatic Imaging Telescope (Filippenko et al. 2001), the Nearby Supernova Factory (Copin et al. 2006), the Center for Astrophysics SN group (Hicken et al. 2009a), the Carnegie Supernova Project (Hamuy et al. 2006; Folatelli et al. 2010), and the Palomar Transient Factory (Law et al. 2009)…”
NORMAL TYPE Ia SUPERNOVAE FROM VIOLENT MERGERS OF WHITE DWARF BINARIES (2012, background): “These values are well within the range of normal SNe Ia (Hicken et al. 2009).”
Observational Clues to the Progenitors of Type Ia Supernovae (2013, background): “…of these scatter plots is likely affected by the different ways of defining light-curve parameters (this is evident from comparing the plot in Hicken et al. (2009), that uses the x1 light-curve stretch parameter, with their plot that uses the ∆ light-curve-width parameter), or by the…”
THE SPECTROSCOPIC DIVERSITY OF TYPE Ia SUPERNOVAE (2000, methodology): “Several large sets of optical SN Ia light curves have already been published (Hamuy et al. 1996; Riess et al. 1999; Jha et al. 2006; Hicken et al. 2009; Contreras et al. 2010; Ganeshalingam et al. 2010; Stritzinger et al. 2011), but until the recent publication of 432 spectra of 32 SN Ia by…”
CONFIRMATION OF A STAR FORMATION BIAS IN TYPE Ia SUPERNOVA DISTANCES AND ITS EFFECT ON THE MEASUREMENT OF THE HUBBLE CONSTANT (2014, methodology): “Accurate SN Ia positions for use in positioning the measurement apertures are taken from Hicken et al. (2009a), Hamuy et al. (1996) or NED.19 The astrometric accuracy of the GALEX data set is 0.”
COSMOLOGICAL CONSTRAINTS FROM MEASUREMENTS OF TYPE Ia SUPERNOVAE DISCOVERED DURING THE FIRST 1.5 yr OF THE Pan-STARRS1 SURVEY (2013, methodology): “We also use the SN Ia compiled more recently by CfA3 (Hicken et al. 2009a, 185 SNe), CSP (Contreras et al. 2010, 85 SNe), and CfA4 (Hicken et al. 2012, 94 SNe).”