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 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:
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FileName Lrecl Records Explanations
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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)
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Byte-by-byte Description of file: tables.dat
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Bytes Format Units Label Explanations
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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.
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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 2007ApJ...659...98R
8 = Cohen et al., 2000, Cat. J/ApJ/538/29
9 = Hornschemeier et al., 2003AJ....126..575H 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).
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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