J/ApJS/262/27 Abundances in inner, outer & FOV of 18 clusters (Batalha+, 2022)
Ranking theoretical supernovae explosion models from observations of the
intracluster gas.
Batalha R.M., Dupke R.A., Jimenez-Teja Y.
<Astrophys. J. Suppl. Ser., 262, 27 (2022)>
=2022ApJS..262...27B 2022ApJS..262...27B
ADC_Keywords: Clusters, galaxy; Intergalactic medium; Abundances; X-ray sources
Keywords: Intracluster medium ; Chemical abundances ; X-ray astronomy ;
Galaxy clusters ; Supernovae
Abstract:
The intracluster medium (ICM) is a reservoir of heavy elements
synthesized by different supernovae (SNe) types over cosmic history.
Different enrichment mechanisms contribute a different relative metal
production, predominantly caused by different SNe type dominance.
Using spatially resolved X-ray spectroscopy, one can probe the
contribution of each metal-enrichment mechanism. However, a large
variety of physically feasible supernova (SN) explosion models make
the analysis of the ICM enrichment history more uncertain. This paper
presents a nonparametric probability distribution function analysis to
rank different theoretical SNe yields models by comparing their
performance against observations. Specifically, we apply this new
methodology to rank 7192 combinations of core-collapse SN and Type Ia
SN models using eight abundance ratios from Suzaku observations of 18
galaxy systems (clusters and groups) to test their predictions. This
novel technique can compare many SN models and maximize spectral
information extraction, considering all the individual measurable
abundance ratios and their uncertainties. We find that Type II SNe
with nonzero initial metallicity progenitors in general performed
better than pair-instability SN and hypernova models, and that 3D SNIa
models (with a white dwarf progenitor central density of
2.9x109g/cm3) performed best among all tested SN model pairs.
Description:
Our analysis is based on 18 nearby (z≤0.0391) groups and clusters of
galaxies observed with the X-ray Imaging Spectrometer (XIS)
observations on board the Suzaku satellite. Observations were
downloaded from the HEASARC website. We selected the observations with
the longest exposure time available for each object in the sample
(see Table 1).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 92 18 Observations of groups and clusters of galaxies
table2.dat 128 54 Error-weighted average of all XIS instruments for
temperature and chemical abundance from inner,
outer, and total (entire) Field of View spectra
regions (see Section 2)
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See also:
J/ApJ/608/405 : Explosive yields of massive star (Chieffi+, 2004)
J/ApJS/182/12 : ICM entropy profiles (ACCEPT) (Cavagnolo+, 2009)
J/ApJ/724/341 : Nucleosynthesis of massive metal-free stars (Heger+, 2010)
http://heasarc.gsfc.nasa.gov/docs/suzaku : Suzaku home page on HEASARC
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Cluster or group name (as in Table 2)
19- 23 A5 --- OName Other designation
25- 26 I2 h RAh Hour of right ascension (J2000)
28- 29 I2 min RAm Minute of right ascension (J2000)
31- 35 F5.2 s RAs Second of right ascension (J2000)
37 A1 --- DE- Sign of declination (J2000)
38- 39 I2 deg DEd Degree of declination (J2000)
41- 42 I2 arcmin DEm Arcminute of declination (J2000)
44- 47 F4.1 arcsec DEs Arcsecond of declination (J2000)
49- 55 F7.5 --- z [0.004/0.04] Redshift from NED to perform
spectral fittings (see Section 2.2)
57- 58 A2 --- l_Rad [≲ ] Limit flag on Rad
59- 61 I3 kpc Rad [10/110] Cool-core radius (1)
63- 71 I9 --- ObsID Observation identifier
73- 77 F5.1 ks Exp [10.8/155.9] Exposure time
79- 92 A14 --- PI Principal Investigator on the proposal
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Note (1): Cool-core Radius indicates the radius that delimits the inner regions
of each group/cluster, i.e., limits the inner region.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Loc Group/cluster location (1)
4- 20 A17 --- Name Name of the groups or cluster
22- 26 F5.3 [kT] Temp [0.7/8.7] Log temperature of the group or cluster
28- 32 F5.3 [kT] e_Temp [0.002/0.08] Uncertainty in Temp
34- 37 F4.2 [Sun] Ar [0.2/2.6] Log abundance of Ar
39- 42 F4.2 [Sun] e_Ar [0.03/1.0] Uncertainty in Ar
44- 47 F4.2 [Sun] Ca [0.03/2.5] Log abundance of Ca
49- 52 F4.2 [Sun] e_Ca [0.02/0.9] Uncertainty in Ca
54- 58 F5.3 [Sun] Fe [0.03/0.9] Log abundance of Fe
60- 64 F5.3 [Sun] e_Fe [0.001/0.1] Uncertainty in Fe
66- 69 F4.2 [Sun] Mg [0.1/1.53] Log abundance of Mg
71- 74 F4.2 [Sun] e_Mg [0.01/0.4] Uncertainty in Mg
76- 79 F4.2 [Sun] Ne [0.05/2.44] Log abundance of Ne
81- 84 F4.2 [Sun] e_Ne [0.02/0.9] Uncertainty in Ne
86- 89 F4.2 [Sun] Ni [0.05/3] Log abundance of Ni
91- 94 F4.2 [Sun] e_Ni [0.03/0.9] Uncertainty in Ni
96- 100 F5.3 [Sun] O [0.009/1.6] Log abundance of O
102- 106 F5.3 [Sun] e_O [0.006/0.3] Uncertainty in O
108- 111 F4.2 [Sun] S [0.24/3] Log abundance of S
113- 116 F4.2 [Sun] e_S [0.01/1] Uncertainty in S
118- 122 F5.3 [Sun] Si [0.24/1.6] Log abundance of Si
124- 128 F5.3 [Sun] e_Si [0.009/0.3] Uncertainty in Si
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Note (1): Location (see Section 2.1) as follows:
IR = Inner region (circles with radii varying from 1' to 4') ;
OR = Outer region (annuli with a radius ≥5');
FV = Full field of view region (8' radius).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 17-Nov-2022