A Linear Relation between the Color Stretch s BV and the Rising Color Slope s0*(B-V) of Type Ia Supernovae

被引：0

作者：

Chen, Ping ^{[1
,2
,3
]}

Dong, Subo ^{[1
]}

Ashall, Chris ^{[4
]}

Benetti, S. ^{[5
]}

Bersier, D. ^{[6
]}

Bose, S. ^{[7
,8
]}

Brimacombe, Joseph ^{[9
]}

Brink, Thomas G. ^{[10
]}

Buckley, David A. H. ^{[11
]}

Cappellaro, Enrico ^{[5
]}

Christie, Grant W. ^{[12
]}

Elias-Rosa, N. ^{[5
,13
]}

Filippenko, Alexei V. ^{[10
]}

Gromadzki, Mariusz ^{[14
]}

Holoien, Thomas W. -S. ^{[15
]}

Hu, Shaoming ^{[16
]}

Kochanek, C. S. ^{[7
,8
]}

Koff, Robert ^{[17
]}

Kollmeier, Juna A. ^{[15
]}

Lundqvist, P. ^{[18
]}

Mattila, S. ^{[19
]}

Milne, Peter A. ^{[20
]}

Munoz, J. A. ^{[21
,22
]}

Mutel, Robert ^{[23
]}

Natusch, Tim ^{[24
]}

Nicolas, Joel ^{[25
]}

Pastorello, A. ^{[5
]}

Prentice, Simon ^{[26
]}

Prieto, J. L. ^{[27
,28
]}

Roth, Tyler ^{[23
]}

Shappee, B. J. ^{[4
]}

Stone, Geoffrey ^{[29
]}

Stanek, K. Z. ^{[7
,8
]}

Stritzinger, M. D. ^{[30
]}

Thompson, Todd A. ^{[7
,8
]}

Tomasella, Lina ^{[5
]}

Villanueva, Steven ^{[31
]}

机构：

[1] Peking Univ, Kavli Inst Astron & Astrophys, Yi He Yuan Rd 5, Beijing 100871, Peoples R China

[2] Peking Univ, Sch Phys, Dept Astron, Yi He Yuan Rd 5, Beijing 100871, Peoples R China

[3] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel

[4] Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA

[5] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[6] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, England

[7] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA

[8] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, 191 W Woodruff Ave, Columbus, OH 43210 USA

[9] Coral Towers Observ, Cairns City, Qld, Australia

[10] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[11] South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa

[12] Auckland Observ, Auckland, New Zealand

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

[14] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

[15] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[16] Shandong Univ, Inst Space Sci, Sch Space Sci & Phys, Shandong Key Lab Opt Astron & Solar Terr Environm, Weihai 264209, Shandong, Peoples R China

[17] Antelope Hills Observ, 980 Antelope Dr West, Bennett, CO 80102 USA

[18] Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden

[19] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-20014 Turku, Finland

[20] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA

[21] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain

[22] Univ Valencia, Observ Astron, E-46980 Valencia, Spain

[23] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA

[24] AUT Univ, IRASR, Auckland, New Zealand

[25] Io Variablles CCD Grp, 364 Chemin Notre Dame, F-06220 Vallauris, France

[26] Univ Dublin, Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland

[27] Univ Diego Portales, Nucleo Astron, Fac Ingn & Ciencias, Ave Ejercito 441, Santiago, Chile

[28] Millennium Inst Astrophys, Santiago, Chile

[29] CBA Sierras, 44325 Alder Hts Rd, Auberry, CA 93602 USA

[30] Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

[31] MIT, Cambridge, MA 02139 USA

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 946卷 / 02期

关键词：

PRECISE DISTANCE; LIGHT CURVES; DATA RELEASE; PROJECT; SN-1991T; MAGNITUDES; DIAGRAM; MAXIMUM; 1991BG;

D O I：

10.3847/1538-4357/acc404

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using data from the Complete Nearby (redshift z (host) < 0.02) sample of Type Ia Supernovae (CNIa0.02), we find a linear relation between two parameters derived from the B - V color curves of Type Ia supernovae: the color stretch s ( BV ) and the rising color slope s(0)*(B-V) BV . The s ( BV ) parameter is known to be tightly correlated with the peak luminosity, especially for fast decliners (dim Type Ia supernovae), and the luminosity correlation with s ( BV ) is markedly better than with the classic light-curve width parameters such as ?m (15)(B). Thus, our new linear relation can be used to infer peak luminosity from s(0)* s ( BV ) (or ?m (15)(B)), the measurement of s(0)*(B-V)

引用

页数：7

共 7 条

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