Concerning colour: The effect of environment on type Ia supernova colour in the dark energy survey

被引：3

作者：

Kelsey, L. ^{[1
,2
]}

Sullivan, M. ^{[2
]}

Wiseman, P. ^{[2
]}

Armstrong, P. ^{[3
]}

Chen, R. ^{[4
]}

Brout, D. ^{[5
]}

Davis, T. M. ^{[6
]}

Dixon, M. ^{[7
]}

Frohmaier, C. ^{[1
,2
]}

Galbany, L. ^{[8
,9
]}

Graur, O. ^{[1
]}

Kessler, R. ^{[10
,11
]}

Lidman, C. ^{[3
,12
]}

Moller, A. ^{[7
]}

Popovic, B. ^{[4
]}

Rose, B. ^{[4
]}

Scolnic, D. ^{[4
]}

Smith, M. ^{[13
]}

Vincenzi, M. ^{[4
]}

Abbott, T. M. C. ^{[14
]}

Aguena, M. ^{[15
]}

Allam, S. ^{[16
]}

Alves, O. ^{[15
,17
]}

Annis, J. ^{[16
]}

Bacon, D. ^{[1
]}

Bertin, E. ^{[18
,19
]}

Bocquet, S. ^{[20
]}

Brooks, D. ^{[21
]}

Burke, D. L. ^{[22
,23
]}

Rosell, A. Carnero ^{[15
,24
,25
]}

Kind, M. Carrasco ^{[26
,27
]}

Carretero, J. ^{[28
]}

Costanzi, M. ^{[29
,30
,31
]}

da Costa, L. N. ^{[15
]}

Pereira, M. E. S. ^{[32
]}

Desai, S. ^{[33
]}

Diehl, H. T. ^{[16
]}

Everett, S. ^{[34
]}

Ferrero, I. ^{[35
]}

Frieman, J. ^{[11
,16
]}

Garcia-Bellido, J. ^{[36
]}

Gruen, D. ^{[20
]}

Gruendl, R. A. ^{[26
,27
]}

Gschwend, J. ^{[15
,37
]}

Gutierrez, G. ^{[16
]}

Hinton, S. R. ^{[6
]}

Hollowood, D. L. ^{[38
]}

Honscheid, K. ^{[39
,40
]}

James, D. J. ^{[5
]}

Kuehn, K. ^{[41
,42
]}

机构：

[1] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[2] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[3] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2601, Australia

[4] Duke Univ, Dept Phys, Durham, NC 27708 USA

[5] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[6] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia

[7] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

[8] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain

[9] CSIC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[10] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[11] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[12] Australian Natl Univ, Coll Sci, Ctr Gravitat Astrophys, Canberra, ACT 2601, Australia

[13] Univ Claude Bernard Lyon 1, Univ Lyon, CNRS, IP2I Lyon,IN2P3,IMR 5822, F-69622 Villeurbanne, France

[14] NSFs Natl Opt Infrared Astron Res Lab, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

[15] Lab Interinst eAstron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[16] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[17] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[18] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

[19] UPMC Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

[20] Ludwig Maximilians Univ Munchen, Univ Observ, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

[21] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[22] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

[23] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[24] Inst Astrofis Canarias, E-38205 Tenerife, Spain

[25] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain

[26] Natl Ctr Supercomp Applicat, Ctr Astrophys Surveys, 1205 West Clark St, Urbana, IL 61801 USA

[27] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[28] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

[29] Univ Trieste, Dept Phys, Astron Unit, Via Tiepolo 11, I-34131 Trieste, Italy

[30] INAF, Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[31] Inst Fundamental Phys Univ, Via Beirut 2, I-34014 Trieste, Italy

[32] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

[33] IIT Hyderabad, Dept Phys, Kandi 502285, Telangana, India

[34] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[35] Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway

[36] Univ Autonoma Madrid, CSIC, Inst Fis Teor UAM, E-28049 Madrid, Spain

[37] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[38] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[39] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[40] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[41] Macquarie Univ, Australian Astron Opt, N Ryde, NSW 2113, Australia

[42] Lowell Observ, 1400 Mars Hill Rd, Flagstaff, AZ 86001 USA

[43] Univ Sydney, Sch Phys, Sydney Inst Astron, A28, Sydney, NSW 2006, Australia

[44] Ctr Invest Energet Medioambient & Tecnol CIEMAT, E-28040 Madrid, Spain

[45] Inst Catalana Recerca & Estudis Avanats, E-08010 Barcelona, Spain

[46] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA

[47] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[48] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[49] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[50] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2022年 / 519卷 / 02期

基金：

欧洲研究理事会; 美国国家科学基金会; 英国科学技术设施理事会;

关键词：

surveys; supernovae: general; distance scale; cosmology: observations; PANTHEON PLUS ANALYSIS; HOST GALAXIES; STAR-FORMATION; SDSS-II; COSMOLOGICAL CONSTRAINTS; HUBBLE RESIDUALS; LEGACY SURVEY; SNE IA; IMPROVED DISTANCES; DUST EXTINCTION;

D O I：

10.1093/mnras/stac3711

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Recent analyses have found intriguing correlations between the colour (c) of type Ia supernovae (SNe Ia) and the size of their 'mass-step', the relationship between SN Ia host galaxy stellar mass (M-stellar) and SN Ia Hubble residual, and suggest that the cause of this relationship is dust. Using 675 photometrically classified SNe Ia from the Dark Energy Survey 5-yr sample, we study the differences in Hubble residual for a variety of global host galaxy and local environmental properties for SN Ia subsamples split by their colour. We find a 3 sigma difference in the mass-step when comparing blue (c < 0) and red (c > 0) SNe. We observe the lowest r.m.s. scatter (similar to 0.14mag) in the Hubble residual for blue SNe in low mass/blue environments, suggesting that this is the most homogeneous sample for cosmological analyses. By fitting for c-dependent relationships between Hubble residuals and M-stellar, approximating existing dust models, we remove the mass-step from the data and find tentative similar to 2 sigma residual steps in rest-frame galaxy U - R colour. This indicates that dust modelling based on M-stellar may not fully explain the remaining dispersion in SN Ia luminosity. Instead, accounting for a c-dependent relationship between Hubble residuals and global U - R, results in <= 1 sigma residual steps in M-stellar and local U - R, suggesting that U - R provides different information about the environment of SNe Ia compared to M-stellar, and motivating the inclusion of galaxy U - R colour in SN Ia distance bias correction.

引用

页码：3046 / 3063

页数：18

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