A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood

The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion...
Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Hossein Fatheddin [verfasserIn] Sedighe Sajadian [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Astrostatistics techniques Stellar dynamics Solar neighborhood

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 945(2023), 1, p 75
Übergeordnetes Werk:	volume:945 ; year:2023 ; number:1, p 75

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/acb548

Katalog-ID:	DOAJ089160657

Internformat


LEADER	01000naa a22002652 4500
001	DOAJ089160657
003	DE-627
005	20230505015850.0
007	cr uuu---uuuuu
008	230505s2023 xx \|\|\|\|\|o 00\| \|\|eng c
024	7		\|a 10.3847/1538-4357/acb548 \|2 doi
035			\|a (DE-627)DOAJ089160657
035			\|a (DE-599)DOAJ470658aadf4e4673b962b989e5771ff7
040			\|a DE-627 \|b ger \|c DE-627 \|e rakwb
041			\|a eng
050		0	\|a QB460-466
100	0		\|a Hossein Fatheddin \|e verfasserin \|4 aut
245	1	2	\|a A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood
264		1	\|c 2023
336			\|a Text \|b txt \|2 rdacontent
337			\|a Computermedien \|b c \|2 rdamedia
338			\|a Online-Ressource \|b cr \|2 rdacarrier
520			\|a The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses.
650		4	\|a Astrostatistics techniques
650		4	\|a Stellar dynamics
650		4	\|a Solar neighborhood
653		0	\|a Astrophysics
700	0		\|a Sedighe Sajadian \|e verfasserin \|4 aut
773	0	8	\|i In \|t The Astrophysical Journal \|d IOP Publishing, 2022 \|g 945(2023), 1, p 75 \|w (DE-627)269019219 \|w (DE-600)1473835-1 \|x 15384357 \|7 nnns
773	1	8	\|g volume:945 \|g year:2023 \|g number:1, p 75
856	4	0	\|u https://doi.org/10.3847/1538-4357/acb548 \|z kostenfrei
856	4	0	\|u https://doaj.org/article/470658aadf4e4673b962b989e5771ff7 \|z kostenfrei
856	4	0	\|u https://doi.org/10.3847/1538-4357/acb548 \|z kostenfrei
856	4	2	\|u https://doaj.org/toc/1538-4357 \|y Journal toc \|z kostenfrei
912			\|a GBV_USEFLAG_A
912			\|a SYSFLAG_A
912			\|a GBV_DOAJ
912			\|a GBV_ILN_11
912			\|a GBV_ILN_20
912			\|a GBV_ILN_22
912			\|a GBV_ILN_23
912			\|a GBV_ILN_24
912			\|a GBV_ILN_31
912			\|a GBV_ILN_39
912			\|a GBV_ILN_40
912			\|a GBV_ILN_60
912			\|a GBV_ILN_62
912			\|a GBV_ILN_63
912			\|a GBV_ILN_65
912			\|a GBV_ILN_69
912			\|a GBV_ILN_70
912			\|a GBV_ILN_73
912			\|a GBV_ILN_95
912			\|a GBV_ILN_105
912			\|a GBV_ILN_110
912			\|a GBV_ILN_151
912			\|a GBV_ILN_161
912			\|a GBV_ILN_170
912			\|a GBV_ILN_230
912			\|a GBV_ILN_285
912			\|a GBV_ILN_293
912			\|a GBV_ILN_370
912			\|a GBV_ILN_602
912			\|a GBV_ILN_702
912			\|a GBV_ILN_2014
912			\|a GBV_ILN_2088
912			\|a GBV_ILN_2522
912			\|a GBV_ILN_4012
912			\|a GBV_ILN_4037
912			\|a GBV_ILN_4046
912			\|a GBV_ILN_4112
912			\|a GBV_ILN_4125
912			\|a GBV_ILN_4126
912			\|a GBV_ILN_4249
912			\|a GBV_ILN_4305
912			\|a GBV_ILN_4306
912			\|a GBV_ILN_4307
912			\|a GBV_ILN_4313
912			\|a GBV_ILN_4322
912			\|a GBV_ILN_4323
912			\|a GBV_ILN_4324
912			\|a GBV_ILN_4325
912			\|a GBV_ILN_4335
912			\|a GBV_ILN_4338
912			\|a GBV_ILN_4367
912			\|a GBV_ILN_4700
951			\|a AR
952			\|d 945 \|j 2023 \|e 1, p 75

Indexfelder

author_variant	h f hf s s ss
matchkey_str	article:15384357:2023----::saitcleainewemsaenvlctdsesoi
hierarchy_sort_str	2023
callnumber-subject-code	QB
publishDate	2023
allfields	10.3847/1538-4357/acb548 doi (DE-627)DOAJ089160657 (DE-599)DOAJ470658aadf4e4673b962b989e5771ff7 DE-627 ger DE-627 rakwb eng QB460-466 Hossein Fatheddin verfasserin aut A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses. Astrostatistics techniques Stellar dynamics Solar neighborhood Astrophysics Sedighe Sajadian verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 945(2023), 1, p 75 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:945 year:2023 number:1, p 75 https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/article/470658aadf4e4673b962b989e5771ff7 kostenfrei https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 945 2023 1, p 75
spelling	10.3847/1538-4357/acb548 doi (DE-627)DOAJ089160657 (DE-599)DOAJ470658aadf4e4673b962b989e5771ff7 DE-627 ger DE-627 rakwb eng QB460-466 Hossein Fatheddin verfasserin aut A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses. Astrostatistics techniques Stellar dynamics Solar neighborhood Astrophysics Sedighe Sajadian verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 945(2023), 1, p 75 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:945 year:2023 number:1, p 75 https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/article/470658aadf4e4673b962b989e5771ff7 kostenfrei https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 945 2023 1, p 75
allfields_unstemmed	10.3847/1538-4357/acb548 doi (DE-627)DOAJ089160657 (DE-599)DOAJ470658aadf4e4673b962b989e5771ff7 DE-627 ger DE-627 rakwb eng QB460-466 Hossein Fatheddin verfasserin aut A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses. Astrostatistics techniques Stellar dynamics Solar neighborhood Astrophysics Sedighe Sajadian verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 945(2023), 1, p 75 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:945 year:2023 number:1, p 75 https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/article/470658aadf4e4673b962b989e5771ff7 kostenfrei https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 945 2023 1, p 75
allfieldsGer	10.3847/1538-4357/acb548 doi (DE-627)DOAJ089160657 (DE-599)DOAJ470658aadf4e4673b962b989e5771ff7 DE-627 ger DE-627 rakwb eng QB460-466 Hossein Fatheddin verfasserin aut A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses. Astrostatistics techniques Stellar dynamics Solar neighborhood Astrophysics Sedighe Sajadian verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 945(2023), 1, p 75 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:945 year:2023 number:1, p 75 https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/article/470658aadf4e4673b962b989e5771ff7 kostenfrei https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 945 2023 1, p 75
allfieldsSound	10.3847/1538-4357/acb548 doi (DE-627)DOAJ089160657 (DE-599)DOAJ470658aadf4e4673b962b989e5771ff7 DE-627 ger DE-627 rakwb eng QB460-466 Hossein Fatheddin verfasserin aut A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses. Astrostatistics techniques Stellar dynamics Solar neighborhood Astrophysics Sedighe Sajadian verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 945(2023), 1, p 75 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:945 year:2023 number:1, p 75 https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/article/470658aadf4e4673b962b989e5771ff7 kostenfrei https://doi.org/10.3847/1538-4357/acb548 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 945 2023 1, p 75
language	English
source	In The Astrophysical Journal 945(2023), 1, p 75 volume:945 year:2023 number:1, p 75
sourceStr	In The Astrophysical Journal 945(2023), 1, p 75 volume:945 year:2023 number:1, p 75
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Astrostatistics techniques Stellar dynamics Solar neighborhood Astrophysics
isfreeaccess_bool	true
container_title	The Astrophysical Journal
authorswithroles_txt_mv	Hossein Fatheddin @@aut@@ Sedighe Sajadian @@aut@@
publishDateDaySort_date	2023-01-01T00:00:00Z
hierarchy_top_id	269019219
id	DOAJ089160657
language_de	englisch
fullrecord	<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000naa a22002652 4500</leader><controlfield tag="001">DOAJ089160657</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230505015850.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">230505s2023 xx \|\|\|\|\|o 00\| \|\|eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.3847/1538-4357/acb548</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)DOAJ089160657</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)DOAJ470658aadf4e4673b962b989e5771ff7</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="050" ind1=" " ind2="0"><subfield code="a">QB460-466</subfield></datafield><datafield tag="100" ind1="0" ind2=" "><subfield code="a">Hossein Fatheddin</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="2"><subfield code="a">A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2023</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Astrostatistics techniques</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stellar dynamics</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Solar neighborhood</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Astrophysics</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Sedighe Sajadian</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">In</subfield><subfield code="t">The Astrophysical Journal</subfield><subfield code="d">IOP Publishing, 2022</subfield><subfield code="g">945(2023), 1, p 75</subfield><subfield code="w">(DE-627)269019219</subfield><subfield code="w">(DE-600)1473835-1</subfield><subfield code="x">15384357</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:945</subfield><subfield code="g">year:2023</subfield><subfield code="g">number:1, p 75</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.3847/1538-4357/acb548</subfield><subfield code="z">kostenfrei</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doaj.org/article/470658aadf4e4673b962b989e5771ff7</subfield><subfield code="z">kostenfrei</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.3847/1538-4357/acb548</subfield><subfield code="z">kostenfrei</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">https://doaj.org/toc/1538-4357</subfield><subfield code="y">Journal toc</subfield><subfield code="z">kostenfrei</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_DOAJ</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_11</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_20</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_22</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_23</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_24</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_31</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_39</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_40</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_60</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_62</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_63</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_65</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_69</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_73</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_95</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_105</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_110</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_151</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_161</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_170</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_230</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_285</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_293</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_370</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_602</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_702</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2014</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2088</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2522</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4012</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4037</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4046</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4112</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4125</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4126</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4249</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4305</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4306</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4307</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4313</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4322</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4323</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4324</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4325</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4335</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4338</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4367</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4700</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">945</subfield><subfield code="j">2023</subfield><subfield code="e">1, p 75</subfield></datafield></record></collection>
callnumber-first	Q - Science
author	Hossein Fatheddin
spellingShingle	Hossein Fatheddin misc QB460-466 misc Astrostatistics techniques misc Stellar dynamics misc Solar neighborhood misc Astrophysics A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood
authorStr	Hossein Fatheddin
ppnlink_with_tag_str_mv	@@773@@(DE-627)269019219
format	electronic Article
delete_txt_mv	keep
author_role	aut aut
collection	DOAJ
remote_str	true
callnumber-label	QB460-466
illustrated	Not Illustrated
issn	15384357
topic_title	QB460-466 A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood Astrostatistics techniques Stellar dynamics Solar neighborhood
topic	misc QB460-466 misc Astrostatistics techniques misc Stellar dynamics misc Solar neighborhood misc Astrophysics
topic_unstemmed	misc QB460-466 misc Astrostatistics techniques misc Stellar dynamics misc Solar neighborhood misc Astrophysics
topic_browse	misc QB460-466 misc Astrostatistics techniques misc Stellar dynamics misc Solar neighborhood misc Astrophysics
format_facet	Elektronische Aufsätze Aufsätze Elektronische Ressource
format_main_str_mv	Text Zeitschrift/Artikel
carriertype_str_mv	cr
hierarchy_parent_title	The Astrophysical Journal
hierarchy_parent_id	269019219
hierarchy_top_title	The Astrophysical Journal
isfreeaccess_txt	true
familylinks_str_mv	(DE-627)269019219 (DE-600)1473835-1
title	A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood
ctrlnum	(DE-627)DOAJ089160657 (DE-599)DOAJ470658aadf4e4673b962b989e5771ff7
title_full	A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood
author_sort	Hossein Fatheddin
journal	The Astrophysical Journal
journalStr	The Astrophysical Journal
callnumber-first-code	Q
lang_code	eng
isOA_bool	true
recordtype	marc
publishDateSort	2023
contenttype_str_mv	txt
author_browse	Hossein Fatheddin Sedighe Sajadian
container_volume	945
class	QB460-466
format_se	Elektronische Aufsätze
author-letter	Hossein Fatheddin
doi_str_mv	10.3847/1538-4357/acb548
author2-role	verfasserin
title_sort	statistical relation between mass, age, and velocity dispersion in the solar neighborhood
callnumber	QB460-466
title_auth	A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood
abstract	The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses.
abstractGer	The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses.
abstract_unstemmed	The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses.
collection_details	GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700
container_issue	1, p 75
title_short	A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood
url	https://doi.org/10.3847/1538-4357/acb548 https://doaj.org/article/470658aadf4e4673b962b989e5771ff7 https://doaj.org/toc/1538-4357
remote_bool	true
author2	Sedighe Sajadian
author2Str	Sedighe Sajadian
ppnlink	269019219
callnumber-subject	QB - Astronomy
mediatype_str_mv	c
isOA_txt	true
hochschulschrift_bool	false
doi_str	10.3847/1538-4357/acb548
callnumber-a	QB460-466
up_date	2024-07-03T21:36:34.294Z
_version_	1803595383356522496
fullrecord_marcxml	<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000naa a22002652 4500</leader><controlfield tag="001">DOAJ089160657</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230505015850.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">230505s2023 xx \|\|\|\|\|o 00\| \|\|eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.3847/1538-4357/acb548</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)DOAJ089160657</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)DOAJ470658aadf4e4673b962b989e5771ff7</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="050" ind1=" " ind2="0"><subfield code="a">QB460-466</subfield></datafield><datafield tag="100" ind1="0" ind2=" "><subfield code="a">Hossein Fatheddin</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="2"><subfield code="a">A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2023</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">The stellar kinematics of the Galactic disk are the main factors constraining disk formation and evolution processes in the Milky Way. In this paper, we investigate a statistical relation between stellar mass, age, and velocity dispersion for stars in the solar neighborhood. Age–velocity dispersion relations, with their applications, have been studied in detail before, but their correlation with mass was mostly neglected. To investigate this relation, we use proper motion data of more than 113,035 stars in the Galactic disk (with solar distances less than 150 pc) provided by the third data release of the Gaia mission, and for stellar mass and age, Gaia's Final Luminosity Age Mass Estimator is implemented. We analyze this data and the correlations between the parameters with random forest regression, which is an ensemble statistical-learning technique. Finally, we show that, by considering stellar mass alongside age, we can determine velocity dispersions with an average relative error and a mean absolute error of about 9% and 2.68 km s ^−1 , respectively. We also find that the correlation of stellar age with velocity dispersion is 3–8 times more than mass, which varies due to the different stellar types and masses.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Astrostatistics techniques</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stellar dynamics</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Solar neighborhood</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Astrophysics</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Sedighe Sajadian</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">In</subfield><subfield code="t">The Astrophysical Journal</subfield><subfield code="d">IOP Publishing, 2022</subfield><subfield code="g">945(2023), 1, p 75</subfield><subfield code="w">(DE-627)269019219</subfield><subfield code="w">(DE-600)1473835-1</subfield><subfield code="x">15384357</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:945</subfield><subfield code="g">year:2023</subfield><subfield code="g">number:1, p 75</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.3847/1538-4357/acb548</subfield><subfield code="z">kostenfrei</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doaj.org/article/470658aadf4e4673b962b989e5771ff7</subfield><subfield code="z">kostenfrei</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.3847/1538-4357/acb548</subfield><subfield code="z">kostenfrei</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">https://doaj.org/toc/1538-4357</subfield><subfield code="y">Journal toc</subfield><subfield code="z">kostenfrei</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_DOAJ</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_11</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_20</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_22</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_23</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_24</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_31</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_39</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_40</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_60</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_62</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_63</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_65</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_69</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_73</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_95</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_105</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_110</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_151</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_161</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_170</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_230</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_285</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_293</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_370</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_602</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_702</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2014</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2088</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2522</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4012</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4037</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4046</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4112</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4125</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4126</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4249</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4305</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4306</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4307</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4313</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4322</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4323</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4324</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4325</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4335</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4338</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4367</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4700</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">945</subfield><subfield code="j">2023</subfield><subfield code="e">1, p 75</subfield></datafield></record></collection>
score	7.3986187

Nicht das Richtige dabei?

Schreiben Sie uns!

A Statistical Relation between Mass, Age, and Velocity Dispersion in the Solar Neighborhood

Nicht das Richtige dabei?

Zugang & Verfügbarkeit

Vorhandene Bände

Nicht das Richtige dabei?