A New Master Supernovae Ia sample and the investigation of the Hubble tension

被引：0

作者：

Dainotti, M. G. ^{[1
,2
,3
,4
]}

De Simone, B. ^{[5
,7
]}

Garg, A. ^{[6
]}

Kohri, K. ^{[1
,2
,5
,8
,9
]}

Bashyalj, A. ^{[10
,11
]}

Aich, A. ^{[12
]}

Mondal, A. ^{[13
]}

Nagataki, S. ^{[14
,15
,16
]}

Montani, G. ^{[17
,21
]}

Jareen, T. ^{[18
]}

Jabir, V. M. ^{[19
]}

Khanjani, S. ^{[20
]}

Bogdan, M. ^{[22
]}

Fraija, N. ^{[23
]}

Pedreira, A. C. C. do E. S. ^{[23
]}

Dejrah, R. H. ^{[24
]}

Singh, A. ^{[25
]}

Parakh, M. ^{[26
]}

Mandal, R. ^{[27
]}

Jarial, K. ^{[28
]}

Lambiase, G.

Sarkar, H. ^{[29
]}

机构：

[1] Natl Astron Observ Japan, Div Sci, 2 Chome-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[2] SOKENDAI, Grad Univ Adv Studies, Hayama, Kanagawa 2400115, Japan

[3] Space Sci Inst, 4765 Walnut St Ste B, Boulder, CO 80301 USA

[4] Univ Nevada, Nevada Ctr Astrophys, 89154,4505 Maryland Pkwy, Las Vegas, NV 80301 USA

[5] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, Italy

[6] Indian Inst Technol, Dept Astron Astrophys & Space Engn, Indore 453552, Madhya Pradesh, India

[7] Univ Salerno, Dipartimento Fis ER Caianiello, INFN, Grp Collegato Salerno,Sez Napoli, Via Giovanni Paolo II,132, I-84084 Fisciano, Salerno, Italy

[8] KEK, IPNS, Theory Ctr, 1-1 Oho, Tsukuba 3050801, Japan

[9] KEK, QUP WPI, 1-1 Oho, Tsukuba 3050801, Japan

[10] Univ Tokyo, Kavli IPMU WPI, UTIAS, Kashiwa, Chiba 2778583, Japan

[11] Tribhuvan Univ Kirtipur, Cent Dept Phys, Kathmandu 44618, Nepal

[12] Pokhara Astron Soc, Pokhara 33700, Nepal

[13] Prayoga Inst Educ Res, Kanakapura Rd, Bengaluru, Karnataka, India

[14] Indian Inst Sci Educ & Res IISER Pune, Dr Homi Bhabha Rd Pashan, Pune 411008, Maharashtra, India

[15] RIKEN Cluster Pioneering Res, Astrophys Big Bang Lab ABBL, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[16] Okinawa Inst Sci & Technol Grad Univ OIST, Sci & Technol Grp, 1919-1 Tancha, Onna Son, Okinawa 9040495, Japan

[17] Sapienza Univ Rome, Phys Dept, Ple Aldo Moro 5, I-00185 Rome, Italy

[18] Thanu Padmanabhan Ctr Cosmol & Sci Popularizat, Gurugram 122505, Haryana, India

[19] Indira Gandhi Natl Tribal Univ IGNTU, Amarkantak 484886, Madhya Pradesh, India

[20] Bahai Inst Higher Educ BIHE, Tehran, Iran

[21] ENEA, Fus & Nucl Safety Dept, Via E Fermi 45, I-00044 Frascati, Italy

[22] Univ Wroclaw, Dept Math, PL-50384 Wroclaw, Poland

[23] Univ Nacl Autonoma Mexico, Inst Astron, Postal 70-264, Mexico City 04510, Mexico

[24] Ankara Univ, Dept Phys, Fac Sci, TR-06100 Ankara, Turkiye

[25] Natl Inst Sci Educ & Res, Bhubaneswar 752050, Odisha, India

[26] Indian Inst Sci Educ & Res Bhopal, Bhopal Bypass Rd, Bhauri 462066, Madhya Pradesh, India

[27] Indian Inst Space Sci & Technol, Dept Earth & Space Sci, Thiruvananthapuram 695547, Kerala, India

[28] Univ Delhi, Sri Venkateswara Coll, Dept Phys, H5Q9 96J,Moti Bagh II, Delhi 110021, India

[29] Indian Inst Sci Educ & Res, Sect 81, Sas Nagar 140306, Punjab, India

来源：

JOURNAL OF HIGH ENERGY ASTROPHYSICS | 2025年 / 48卷

关键词：

Cosmology; SNe Ia; Hubble constant; Hubble tension; GAMMA-RAY BURSTS; TULLY-FISHER RELATION; DARK ENERGY; LAMBDA-CDM; INDEPENDENT DETERMINATION; ACOUSTIC-OSCILLATIONS; COSMOLOGICAL ANALYSIS; CONSTANT; MODEL; H-0;

D O I：

10.1016/j.jheap.2025.100405

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Modern cosmological research still thoroughly debates the discrepancy between local probes and the Cosmic Microwave Background observations in the Hubble constant (H0) measurements, ranging from 4 to 6 sigma. In the current study, we examine this tension using the Supernovae Ia (SNe Ia) data from the Pantheon, Pantheon+ (P+), Joint Lightcurve Analysis (JLA), and Dark Energy Survey, (DES) catalogs combined together into the so-called Master Sample. The sample contains 3714 SNe Ia, and is divided all of them into redshift-ordered bins. Three binning techniques are presented: the equi-population, the moving window (MW), and the equi-spacing in the log -z. We perform a Markov-Chain Monte Carlo analysis (MCMC) for each bin to determine the H-0 value, estimating it within the standard flat Lambda CDM and the w(0)w(a)CDM models. These H0 values are then fitted with the following phenomenological function: H-0(z)=H-0/(1+z)(alpha), where H-0 is a free parameter representing H-0(z) fitted in z=0, and alpha is the evolutionary parameter. Our results indicate a decreasing trend characterized by alpha similar to 0.01, whose consistency with zero ranges from 1 sigma in 5 cases to 1 case at 3 sigma and 11 cases at >3 sigma in several samples and configurations. Such a trend in the SNe Ia catalogs could be due to evolution with redshift for the astrophysical variables or unveiled selection biases. Alternatively, intrinsic physics, possibly the f(R) theory of gravity, could be responsible for this trend.

引用

页数：38

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