J/ApJ/673/981 Type Ia supernova rates with HST ACS (Kuznetsova+, 2008)
A new determination of the high-redshift type Ia supernova rates with the Hubble Space Telescope Advanced Camera for Surveys. Kuznetsova N., Barbary K., Connolly B., Kim A.G., Pain R., Roe N.A., Aldering G., Amanullah R., Dawson K., Doi M., Fadeyev V., Fruchter A.S., Gibbons R., Goldhaber G., Goobar A., Gude A., Knop R.A., Kowalski M., Lidman C., Morokuma T., Meyers J., Perlmutter S., Rubin D., Schlegel D.J., Spadafora A.L., Stanishev V., Strovink M., Suzuki N., Wang L., Yasuda N., (Supernova Cosmology Project) <Astrophys. J., 673, 981-998 (2008)> =2008ApJ...673..981K
ADC_Keywords: Supernovae ; Redshifts Keywords: supernovae: general Abstract: We present a new measurement of the volumetric rate of SNe Ia up to a redshift of 1.7, using the HST GOODS data combined with an additional HST data set covering the GOODS-North field collected in 2004. We employ a novel technique that does not require spectroscopic data for identifying SNe Ia (although spectroscopic measurements of redshifts are used for over half the sample); instead, we employ a Bayesian approach using only photometric data to calculate the probability that an object is an SN Ia. This Bayesian technique can easily be modified to incorporate improved priors on SN properties, and it is well-suited for future high-statistics SN searches in which spectroscopic follow-up of all candidates will be impractical. Here the method is validated on both ground- and space-based SN data having some spectroscopic follow-up. We combine our volumetric rate measurements with low-redshift SN data and fit to a number of possible models for the evolution of the SN Ia rate as a function of redshift. The data do not distinguish between a flat rate at redshift >0.5 and a previously proposed model, in which the Type Ia rate peaks at redshift ∼1 due to a significant delay from star formation to the SN explosion. Except for the highest redshifts, where the signal-to-noise ratio is generally too low to apply this technique, this approach yields uncertainties that are smaller than or comparable to previous work. Description: For this analysis, we use the HST GOODS data set collected in 2002-2003. In addition to the GOODS data, we use an HST sample collected in the spring and summer of 2004, which we hereafter call the 2004 Advanced Camera for Surveys (ACS) sample. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tables.dat 93 57 Candidates Selected at the end of stage 2 for Samples 1, 2, 3 and 4 (tables 4-7 of the paper)
Byte-by-byte Description of file: tables.dat
Bytes Format Units Label Explanations
1 I1 --- Sam [1/4] Sample number 3- 4 I2 --- Cand Candidate number (1) 6- 7 I2 h RAh Right ascension (J2000.0) 9- 10 I2 min RAm Right ascension (J2000.0) 12- 17 F6.3 s RAs Right ascension (J2000.0) 19 A1 --- DE- Declination sing (J2000.0) 20- 21 I2 deg DEd Declination (J2000.0) 23- 24 I2 arcmin DEm Declination (J2000.0) 26- 30 F5.2 arcsec DEs Declination (J2000.0) 32- 36 F5.3 --- z ? Redshift 37 A1 --- n_z [:u] Uncertainty flag or u for Unconstrained (2) 39- 43 F5.3 --- e_z ? rms uncertainty on z 45- 58 A14 --- Source Sources used for the redshift and redshift error determination 61- 64 A4 --- r_z References for the sources (3) 66- 86 A21 --- Com Comments (4) 90- 92 F3.1 --- Prob ? Probability of SN Ia type 93 A1 --- n_Prob [n] n stands for a special category of candidates designated as "anomalies," as described in Sect. 3.3.
Note (1): Sources identified as [KBC2008] N NN. Note (2): * The redshift of candidate "2 17" is uncertain, as the possible host galaxy is 7" away. Leaving this redshift as unconstrained does not change our results. * The redshift of candidate "3 4" is uncertain, as the possible host galaxy is 4" away. Leaving this redshift as unconstrained does not change our results. Note (3): References as follows: 1 = B. Mobasher & T. Dahlen 2004, private communication; 2 = Cowie et al., 2004, Cat. J/AJ/127/3137 3 = Strolger et al. 2004, Cat. J/ApJ/613/200 4 = Wirth et al. 2004, Cat. J/AJ/127/3121 5 = Riess et al., 2004, Cat. J/ApJ/607/665 6 = this paper 7 = Riess et al., 2007ApJ...659...98R 8 = Cohen et al., 2000, Cat. J/ApJ/538/29 9 = Hornschemeier et al., 2003AJ....126..575H 10 = Le Fevre et al., 2004, Cat. J/A+A/428/1043 11 = Wolf et al. 2004, Cat. II/253 12 = Vanzella et al. 2006, Cat. J/A+A/454/423 Note (4): For the candidates found in Riess et al. (2004, Cat. J/ApJ/607/665) the tables also list the SN name and classification (gold, silver, or bronze).
History: 23-May-2010: From electronic version of the journal 19-Nov-2010: (JST04Yow) corrected into (HST04Yow) in tables.dat file 18-Apr-2012: Candidate #5 added to Sample 4, in tables.dat file
(End) Patricia Vannier [CDS] 09-Apr-2010
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