J/MNRAS/434/1443 SN Ia inside rich galaxy clusters (Xavier+, 2013)
Properties of type Ia supernovae inside rich galaxy clusters.
Xavier H.S., Gupta R.R., Sako M., D'andrea C.B., Frieman J.A., Galbany L.,
Garnavich P.M., Marriner J., Nichol R.C., Olmstead M.D., Schneider D.P.,
Smith M.
<Mon. Not. R. Astron. Soc., 434, 1443-1459 (2013)>
=2013MNRAS.434.1443X 2013MNRAS.434.1443X
ADC_Keywords: Clusters, galaxy ; Supernovae
Keywords: supernovae: general - galaxies: clusters: general
Abstract:
We used the Gaussian Mixture Brightest Cluster Galaxy catalogue and
Sloan Digital Sky Survey-II supernovae data with redshifts measured by
the Baryon Oscillation Spectroscopic Survey to identify 48 Type Ia
supernovae (SNe Ia) residing in rich galaxy clusters and compare their
properties with 1015 SNe Ia in the field. Their light curves were
parametrized by the SALT2 model and the significance of the observed
differences was assessed by a resampling technique. To test our
samples and methods, we first looked for known differences between SNe
Ia residing in active and passive galaxies. We confirm that passive
galaxies host SNe Ia with smaller stretch, weaker colour-luminosity
relation [β of 2.54(22) against 3.35(14)], and that are ∼ 0.1mag
more luminous after stretch and colour corrections. We show that only
0.02 percent of random samples drawn from our set of SNe Ia in active
galaxies can reach these values. Reported differences in the Hubble
residuals scatter could not be detected, possibly due to the exclusion
of outliers. We then show that, while most field and cluster SNe Ia
properties are compatible at the current level, their stretch
distributions are different (∼3σ): besides having a higher
concentration of passive galaxies than the field, the cluster's
passive galaxies host SNe Ia with an average stretch even smaller than
those in field passive galaxies (at 95 percent confidence). We argue
that the older age of passive galaxies in clusters is responsible for
this effect since, as we show, old passive galaxies host SNe Ia with
smaller stretch than young passive galaxies (∼4σ).
Description:
The SNe data set used in this work was obtained by the SDSS-II
Supernova Survey over the region of the sky called Stripe 82, an
equatorial stripe with declination -1.264°<DE<+1.26° and right
ascension -60°<RA<+60° (York et al. 2000AJ....120.1579Y 2000AJ....120.1579Y;
Frieman et al. 2008AJ....135..338F 2008AJ....135..338F). The Stripe 82 was imaged on all
ugriz filters every four days, on average, during the fall seasons of
2005-2007.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 160 48 All supernovae Ia in the cluster sample
--------------------------------------------------------------------------------
See also:
J/AJ/135/348 : SDSS-II SNe survey: search and follow-up (Sako+, 2008)
J/AJ/135/1766 : Sloan Digital Sky Survey-II supernova survey (Zheng+, 2008)
J/AJ/136/2306 : SDSS-II Supernova survey, 2005 (Holtzman+, 2008)
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 (Kessler+, 2009)
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- CID [822/20882] SN Ia's candidate ID
<SDSS-II SN NNNNN> in Simbad
7- 14 F8.4 deg RAdeg [-90/90] SN right ascension (J2000.0)
16- 22 F7.4 deg DEdeg SN declination (J2000.0)
24- 29 F6.4 --- zsn [0.1/0.44] Supernova redshift zSN
31 A1 --- f_zsn [SPB] Typing kind (S=spectroscopic) (1)
32- 50 I19 --- BCGid Identifier (SDSS objID of its BCG) of the
GMBCG cluster hosting the supernova (Hao et
al. 2010, J/ApJS/191/254)
52- 56 F5.2 --- x1 [-4/3] SALT2 'stretch' parameter x1 (4)
58- 61 F4.2 --- e_x1 rms uncertainty on x1
63- 68 F6.3 --- c [-0.3/0.4] SALT2 'colour' parameter c (4)
70- 73 F4.3 --- e_c rms uncertainty on c
75- 79 F5.2 --- HR Hubble Residual obtained with the full sample
(cluster + field) nuisance parameters (4)
81- 83 F3.2 --- e_HR rms uncertainty on HR
85-103 I19 --- Host ? SDSS-DR8 objID of its host galaxy (2)
105-110 F6.3 Gyr Age ? Age (3)
112-115 F4.2 Gyr E_Age ? Error on Age (upper value)
117-120 F4.2 Gyr e_Age ? Error on Age (lower value)
122-127 F6.3 [Msun] logM ? Mass (3)
129-133 F5.3 [Msun] E_logM ? Error on logM (upper value)
135-139 F5.3 [Msun] e_logM ? Error on logM (lower value)
141-147 F7.3 [yr-1] sSFR ? Specific star formation rate (3)
149-153 F5.3 [yr-1] E_sSFR ? Error on sSFR (upper value)
155-160 F6.3 [yr-1] e_sSFR ? Error on sSFR (lower value)
--------------------------------------------------------------------------------
Note (1): Typing kind as follows:
S = spectroscopic typing
P = photometric typing with host's spec-z from SDSS-II
B = photometric typing with host's spec-z from BOSS
Note (2): Rows with no value correspond to SN Ia with no identifiable host.
Note (3): Rows with no value correspond to hosts that did not pass the
χ2 minimum probability cut.
Note (4): The lightcurves of the supernovae are fitted with the SALT2
model of Guy et al. (2007A&A...466...11G 2007A&A...466...11G) which relates the distance
modulus µ=5log(r/10pc) with the peak B-band apparent magnitude mB
of the supernova, the stretch parameter x1 (supernovae with a wider
light curve [x1>0] are brighter), and the colour parameter c (redder
supernovae [c>0] are dimmer)as: µ=mB-M+αx1_βc,
where α and β are called the "nuisance parameters". The
"Hubble Residual" (HR) is the difference between the distance modulus
obtained with this relation (µSN) and the distance modulus µz
obtained with the cosmology (Ωm=0.27, {Pmega}_Λ=0.73,
Ho=70km/s/Mpc).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 08-Sep-2014