J/ApJ/745/31 HST Cluster Supernova Survey. VI. SNIa rate (Barbary+, 2012)
The Hubble Space Telescope Cluster Supernova Survey.
VI. The volumetric type Ia supernova rate.
Barbary K., Aldering G., Amanullah R., Brodwin M., Connolly N.,
Dawson K.S., Doi M., Eisenhardt P., Faccioli L., Fadeyev V., Fakhouri H.K.,
Fruchter A.S., Gilbank D.G., Gladders M.D., Goldhaber G., Goobar A.,
Hattori T., Hsiao E., Huang X., Ihara Y., Kashikawa N., Koester B.,
Konishi K., Kowalski M., Lidman C., Lubin L., Meyers J., Morokuma T.,
Oda T., Panagia N., Perlmutter S., Postman M., Ripoche P., Rosati P.,
Rubin D., Schlegel D.J., Spadafora A.L., Stanford S.A., Strovink M.,
Suzuki N., Takanashi N., Tokita K., Yasuda N.,
(the Supernova Cosmology Project)
<Astrophys. J., 745, 31 (2012)>
=2012ApJ...745...31B 2012ApJ...745...31B
ADC_Keywords: Supernovae ; Surveys ; Redshifts ; Models
Keywords: cosmology: observations - supernovae: general - white dwarfs
Abstract:
We present a measurement of the volumetric Type Ia supernova (SN Ia)
rate out to z≃1.6 from the Hubble Space Telescope Cluster Supernova
Survey. In observations spanning 189 orbits with the Advanced Camera
for Surveys we discovered 29 SNe, of which approximately 20 are SNe
Ia. Twelve of these SNe Ia are located in the foregrounds and
backgrounds of the clusters targeted in the survey. Using these new
data, we derive the volumetric SN Ia rate in four broad redshift bins,
finding results consistent with previous measurements at z≳1 and
strengthening the case for an SN Ia rate that is
≳0.6x10-4h370/yr/Mpc3 at z∼1 and flattening out at higher
redshift. We provide SN candidates and efficiency calculations in a
form that makes it easy to rebin and combine these results with other
measurements for increased statistics. Finally, we compare the
assumptions about host-galaxy dust extinction used in different
high-redshift rate measurements, finding that different assumptions
may induce significant systematic differences between measurements.
Description:
The details of the HST Cluster SN Survey are described in Dawson et
al. (2009AJ....138.1271D 2009AJ....138.1271D). Briefly, the survey targeted 25 massive
galaxy clusters in a rolling SN search between 2005 July and 2006
December. Clusters were selected from X-ray, optical, and IR surveys
and cover the redshift range 0.9<z<1.46. During the survey, each
cluster was observed once every 20-26 days during its HST visibility
window (typically four to seven months) using ACS.
table2.dat file is the data behind Figure 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 66 273 Figure 2 data behind the figure
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See also:
J/ApJ/723/47 : IfA Deep SN rates (Rodney+, 2010)
J/ApJ/713/1026 : SN Ia rate at redshift ≲0.3 from SDSS-II (Dilday+, 2010)
J/ApJS/185/32 : First-year SDSS-II SN results (K09) (Kessler+, 2009)
J/ApJ/673/981 : Type Ia supernova rates with HST ACS (Kuznetsova+, 2008)
J/ApJ/686/749 : Improved cosmological constraints from SNe (Kowalski+, 2008)
http://supernova.lbl.gov/2009ClusterSurvey/ : Supernova cosmology project
page for the HST Cluster Supernova Survey
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1 I1 --- ID [0/6] Unique integer for each control
time simulation
3- 14 A12 --- Label Description unique to each ID (1)
16- 27 E12.6 --- z [0.05/1.95] Redshift
29- 40 E12.6 yr.arcmin2 t*area [1.3/118.9] Observer-frame control
time x area at z
42- 53 E12.6 --- z2 [0.1/2] Second redshift
55- 66 E12.6 yr.Mpc3 t*vol [57/6581] Total rest-frame control
time x volume between z and z2
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Note (1): Model label as follows:
Dust Model A = used for the main result in Dahlen et al. (2008ApJ...681..462D 2008ApJ...681..462D).
It is based on the model of Hatano et al. (1998ApJ...502..177H 1998ApJ...502..177H)
constructed to estimate extinction in local disk galaxies.
See equation (5) in section 4.3.
Dust Model B = is used by Dahlen et al. (2008ApJ...681..462D 2008ApJ...681..462D) as an alternative
distribution. It is based on the models in Riello & Patat
(2005MNRAS.362..671R 2005MNRAS.362..671R). See equation (6) in section 4.3.
Dust Model C = is used in the rate analysis of Neill et al.
(2006AJ....132.1126N 2006AJ....132.1126N). See equation (7) in section 4.3.
Minimal Dust = In addition to the three distributions A, B and C, we also
consider a distribution with minimal dust, where we assume the
SNLS z<0.6 sample is complete and fit it with a skewed Gaussian
distribution.
K09 Dust = Kessler et al. 2009, Cat. J/ApJS/185/32, extinction model
See section 4 for further explanations.
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History:
From electronic version of the journal
References:
Dawson et al. Paper I. 2009AJ....138.1271D 2009AJ....138.1271D
Barbary et al. Paper II. 2012ApJ...745...32B 2012ApJ...745...32B
Meyers et al. Paper III. 2012ApJ...750....1M 2012ApJ...750....1M
Ripoche et al. Paper IV. ApJ, submitted
Suzuki et al. Paper V. 2012ApJ...746...85S 2012ApJ...746...85S
(End) Greg Schwarz [AAS] , Emmanuelle Perret [CDS] 23-Jul-2013