Astronomy and Astrophysics, volume 479, 49-66 (2008/2-3)
Supernova rates from the Southern inTermediate Redshift ESO Supernova Search (STRESS).
BOTTICELLA M.T., RIELLO M., CAPPELLARO E., BENETTI S., ALTAVILLA G., PASTORELLO A., TURATTO M., GREGGIO L., PATAT F., VALENTI S., ZAMPIERI L., HARUTYUNYAN A., PIGNATA G. and TAUBENBERGER S.
Abstract (from CDS):
To measure the supernova (SN) rates at intermediate redshift we performed a search, the Southern inTermediate Redshift ESO Supernova Search (STRESS). Unlike most of the current high redshift SN searches, this survey was specifically designed to estimate the rate for both type Ia and core collapse (CC) SNe. We counted the SNe discovered in a selected galaxy sample measuring SN rate per unit blue band luminosity. Our analysis is based on a sample of ∼43000 galaxies and on 25 spectroscopically confirmed SNe plus 64 selected SN candidates. Our approach is aimed at obtaining a direct comparison of the high redshift and local rates and at investigating the dependence of the rates on specific galaxy properties, most notably their colour. The type Ia SN rate, at mean redshift z=0.3, is 0.22(+0.10+0.16)(–0.08–0.14)h702SNu, while the CC SN rate, at z=0.21, is 0.82(+0.31+0.30)(–0.24–0.26)h702SNu. The quoted errors are the statistical and systematic uncertainties. With respect to the local value, the CC SN rate at z=0.2 is higher by a factor of ∼2, whereas the type Ia SN rate remains almost constant. This implies that a significant fraction of SN Ia progenitors has a lifetime longer than 2-3Gyr. We also measured the SN rates in the red and blue galaxies and found that the SN Ia rate seems to be constant in galaxies of different colour, whereas the CC SN rate seems to peak in blue galaxies, as in the local Universe. SN rates per unit volume were found to be consistent with other measurements showing a steeper evolution with redshift for CC SNe than SNe Ia. We have exploited the link between SFH and SN rates to predict the evolutionary behaviour of the SN rates and compare it with the path indicated by observations. We conclude that in order to constrain the mass range of CC SN progenitors and SN Ia progenitor models it is necessary to reduce the uncertainties in the cosmic SFH. In addition it is important to apply a consistent dust extinction correction both to SF and to CC SN rate and to measure the SN Ia rate in star forming and in passively evolving galaxies over a wide redshift range.
supernovae: general - stars: formation - Galaxy: evolution - Galaxy: stellar content
VizieR on-line data:
<Available at CDS (J/A+A/479/49): table1.dat table3.dat table45.dat>
Tables 4, 5: STRESS NNZN-A, STRESS EF0427-A, STRESS EisA1-AA, STRESS EisA-A, STRESS WHNN-A, STRESS WHhz2-A, STRESS Field2-A, STRESS J1888-A, N=22+41.
Status at CDS
All or part of tables of objects could be ingested in SIMBAD with priority 2.
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