2018A&A...615A.162L


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET21:49:44

2018A&A...615A.162L - Astronomy and Astrophysics, volume 615A, 162-162 (2018/7-1)

Correcting for peculiar velocities of Type Ia supernovae in clusters of galaxies.

LEGET P.-F., PRUZHINSKAYA M.V., CIULLI A., GANGLER E., ALDERING G., ANTILOGUS P., ARAGON C., BAILEY S., BALTAY C., BARBARY K., BONGARD S., BOONE K., BUTON C., CHILDRESS M., CHOTARD N., COPIN Y., DIXON S., FAGRELIUS P., FEINDT U., FOUCHEZ D., GRIS P., HAYDEN B., HILLEBRANDT W., HOWELL D.A., KIM A., KOWALSKI M., KUESTERS D., LOMBARDO S., LIN Q., NORDIN J., PAIN R., PECONTAL E., PEREIRA R., PERLMUTTER S., RABINOWITZ D., RIGAULT M., RUNGE K., RUBIN D., SAUNDERS C., SAYS L.-P., SMADJA G., SOFIATTI C., SUZUKI N., TAUBENBERGER S., TAO C., THOMAS R.C. (The Nearby Supernova Factory Collaboration)

Abstract (from CDS):


Context. Type Ia supernovae (SNe Ia) are widely used to measure the expansion of the Universe. To perform such measurements the luminosity and cosmological redshift (z) of the SNe Ia have to be determined. The uncertainty on z includes an unknown peculiar velocity, which can be very large for SNe Ia in the virialized cores of massive clusters.
Aims. We determine which SNe Ia exploded in galaxy clusters using 145 SNe Ia from the Nearby Supernova Factory. We then study how the correction for peculiar velocities of host galaxies inside the clusters improves the Hubble residuals.
Methods. We found 11 candidates for membership in clusters. We applied the biweight technique to estimate the redshift of a cluster. Then, we used the galaxy cluster redshift instead of the host galaxy redshift to construct the Hubble diagram.
Results. For SNe Ia inside galaxy clusters, the dispersion around the Hubble diagram when peculiar velocities are taken into account is smaller compared with a case without peculiar velocity correction, which has a wRMS=0.130±0.038mag instead of wRMS=0.137±0.036mag. The significance of this improvement is 3.58σ. If we remove the very nearby Virgo cluster member SN2006X (z<0.01) from the analysis, the significance decreases to 1.34σ. The peculiar velocity correction is found to be highest for the SNe Ia hosted by blue spiral galaxies. Those SNe Ia have high local specific star formation rates and smaller stellar masses, which is seemingly counter to what might be expected given the heavy concentration of old, massive elliptical galaxies in clusters.
Conclusions. As expected, the Hubble residuals of SNe Ia associated with massive galaxy clusters improve when the cluster redshift is taken as the cosmological redshift of the supernova. This fact has to be taken into account in future cosmological analyses in order to achieve higher accuracy for cosmological redshift measurements. We provide an approach to do so.

Abstract Copyright: © ESO 2018

Journal keyword(s): supernovae: general - galaxies: clusters: general - galaxies: distances and redshifts - dark energy

Simbad objects: 40

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Number of rows : 40

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 ACO 76 ClG 00 40 16.1031 +06 52 46.226           ~ 127 2
2 SNF 20061020-000 SN* 00 41 05.192 +06 47 44.34           SNIa 6 0
3 2MASX J00410521+0647439 GiC 00 41 05.216 +06 47 43.96   16.78       ~ 5 0
4 ACO 85 ClG 00 41 37.8 -09 20 33           ~ 797 0
5 PTF 09foz SN* 00 42 11.893 -09 52 54.65   17.81 17.78 18.8   ~ 13 0
6 2MASX J00421192-0952551 GiC 00 42 11.922 -09 52 55.17     16.46     ~ 9 0
7 ACO 87 ClG 00 43 01 -09 47.6           ~ 45 0
8 ACO 119 ClG 00 56 16.8 -01 15 00           ~ 521 2
9 SN 2007nq SN* 00 57 33.60 -01 23 19.5     17.6     SNIa 28 1
10 UGC 595 AGN 00 57 34.920 -01 23 27.89   14.07 15.10     ~ 231 1
11 SN 2005eu SN* 02 27 43.30 +28 10 37.8     17.6     SNIa 50 2
12 LEDA 5065173 G 02 27 43.33 +28 10 37.4           ~ 6 1
13 BAX 037.0388+28.1825 ClG 02 28 09.6 +28 11 39           ~ 12 0
14 SN 2006X SN* 12 22 53.93 +15 48 32.0     15.3     SNIa 284 1
15 M 100 AGN 12 22 54.9318850854 +15 49 20.294302163 10.04 10.05 9.35     ~ 1673 2
16 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5929 0
17 NAME LOCAL SUPERCL SCG 12 31 +12.4           ~ 456 0
18 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4287 2
19 [WHL2012] J132045.4+211627 ClG 13 20 45.35 +21 16 27.1           ~ 3 0
20 SNF 20070417-002 SN* 13 20 52.243 +21 19 45.71           ~ 2 0
21 SNF 20060609-002 SN* 16 04 30.45 +17 28 07.3           ~ 3 0
22 MCG+03-41-072 GiC 16 04 30.450 +17 28 09.20   15       ~ 43 0
23 ACO 2151 ClG 16 05 15.0 +17 44 55           ~ 558 3
24 2MASX J16152860+1913344 G 16 15 28.6 +19 13 34           ~ 4 0
25 SNF 20080612-003 SN* 16 15 28.72 +19 13 32.8           SNIa 5 1
26 1RXS J161531.4+192754 ClG 16 15 34.7 +19 27 36           ~ 8 0
27 SNF 20080731-000 SN* 17 44 03.38 +33 02 24.7           ~ 2 0
28 ZwCl 1742+3306 ClG 17 44 16.2753 +32 59 55.115           ~ 62 0
29 ZwCl 1810+4949 ClG 18 11 00.1 +49 54 40     14.8     ~ 48 0
30 WINGS J181139.70+501057.1 EmG 18 11 39.667 +50 10 57.24           ~ 3 0
31 SNF 20080623-001 SN* 18 11 39.79 +50 10 56.2           SNIa 6 0
32 ZwCl 2259+0746 ClG 23 02.1 +08 02           ~ 5 0
33 1RXS J230215.3+080159 X 23 02 15.300 +08 01 59.02           ~ 2 0
34 BAX 346.7154-13.4164 ClG 23 06 51.7 -13 24 59           ~ 8 0
35 SNF 20061111-002 SN* 23 07 18.69 -13 31 07.3           SNIa 3 0
36 NGC 7647 BiC 23 23 57.414 +16 46 37.94   14.61 14.45     ~ 71 1
37 SN 2009hi SN* 23 23 57.450 +16 46 38.08           SNIa 8 1
38 ACO 2589 ClG 23 24 00.5 +16 49 29           ~ 297 1
39 NAME CFA Great Wall SCG ~ ~           ~ 121 0
40 NAME Local Group GrG ~ ~           ~ 7111 0

    Equat.    Gal    SGal    Ecl

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2020.11.28-21:49:44

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