Photometric and Kinematic Study of the Open Clusters SAI 44 and SAI 45
We carry out a detailed photometric and kinematic study of the poorly studied sparse open clusters SAI 44 and SAI 45 using ground-based BVR c I c data supplemented by archival data from Gaia eDR3 and Pan-STARRS. The stellar memberships are determined using a statistical method based on Gaia eDR3 kin...
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| Veröffentlicht in: | The Astronomical journal 2021-08, Vol.162 (2), p.64 |
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| creator | Maurya, Jayanand Joshi, Y. C. Elsanhoury, W. H. Sharma, Saurabh |
| description | We carry out a detailed photometric and kinematic study of the poorly studied sparse open clusters SAI 44 and SAI 45 using ground-based
BVR
c
I
c
data supplemented by archival data from Gaia eDR3 and Pan-STARRS. The stellar memberships are determined using a statistical method based on Gaia eDR3 kinematic data, and we found 204 members in SAI 44 while only 74 members are identified in SAI 45. The average distances to SAI 44 and SAI 45 are calculated to be 3670 ± 184 and 1668 ± 47 pc. The logarithmic age of the clusters are determined to be 8.82 ± 0.10 and 9.07 ± 0.10 yr for SAI 44 and SAI 45, respectively. The color–magnitude diagram of SAI 45 hosts an extended main-sequence turnoff (eMSTO). The apparent age spread is found to be similar to the apparent age spread predicted on the basis of the age spread and cluster age relation predicted by rotation models. This indicates that eMSTO is a stellar evolution rather than star formation phenomenon in SAI 45. We conclude that eMSTO in SAI 45 is mainly caused by the different rotation rates of stars as the SYCLIST synthetic population with different rotation rates was able to reproduce the observed eMSTO, and stars in the red part of the eMSTO were preferentially concentrated in the inner region, which again hints at different rotations being the reason for the extension in the upper MS. This finding supports the theory attributing the origin of eMSTO to the different rotations of eMSTO stars. The mass function slopes are obtained as −2.24 ± 0.66 and −2.58 ± 3.20 in the mass rages 2.426–0.990
M
⊙
and 2.167–1.202
M
⊙
for SAI 44 and SAI 45, respectively. SAI 44 exhibits the signature of mass segregation while we found weak evidence of mass segregation in SAI 45 possibly due to tidal stripping. The dynamical relaxation times of these clusters indicate that both clusters are in a dynamically relaxed state. Using the AD-diagram method, the apex coordinates are found to be (
69
.°
79
±
0
.°
11
, −
30
.°
82
±
0
.°
15
) for SAI 44 and (−
56
.°
22
±
0
.°
13
, −
56
.°
62
±
0
.°
13
) for SAI 45. The average space velocity components of the clusters SAI 44 and SAI 45 are calculated in units of km s
−1
as (−15.14 ± 3.90, −19.43 ± 4.41, −20.85 ± 4.57) and (28.13 ± 5.30, −9.78 ± 3.13, −19.59 ± 4.43), respectively. |
| doi_str_mv | 10.3847/1538-3881/ac0138 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_O3W</sourceid><recordid>TN_cdi_proquest_journals_2553326434</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2553326434</sourcerecordid><originalsourceid>FETCH-LOGICAL-c378t-edb24caeb98cbc254865f45e7e6bae19b24c56fb1e0546c5dd6012173040c64b3</originalsourceid><addsrcrecordid>eNp1kDtPwzAUhS0EEqWwM1piJXAdP-KOVUWholKRCrOVODdqqjYOtjv035M0iE5M9_Wdo6tDyD2DJ65F9swk1wnXmj3nFhjXF2T0t7okIwAQiUqluiY3IWwBGNMgRmT-sXHR7TH62tK8Kel73eA-j920jofySF1F4wbpqsWGznaHENEHup4uqBAn_tTKW3JV5buAd791TL7mL5-zt2S5el3MpsvE8kzHBMsiFTbHYqJtYVMptJKVkJihKnJkk_4qVVUwBCmUlWWpgKUs4yDAKlHwMXkYfF2ItQm2jmg31jUN2mhSzuSEMzhTrXffBwzRbN3BN91jJpWS81QJLjoKBsp6F4LHyrS-3uf-aBiYPlPTB2j6AM2QaSd5HCS1a8-e_-I_FlxzpA</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2553326434</pqid></control><display><type>article</type><title>Photometric and Kinematic Study of the Open Clusters SAI 44 and SAI 45</title><source>IOP Publishing Free Content</source><creator>Maurya, Jayanand ; Joshi, Y. C. ; Elsanhoury, W. H. ; Sharma, Saurabh</creator><creatorcontrib>Maurya, Jayanand ; Joshi, Y. C. ; Elsanhoury, W. H. ; Sharma, Saurabh</creatorcontrib><description>We carry out a detailed photometric and kinematic study of the poorly studied sparse open clusters SAI 44 and SAI 45 using ground-based
BVR
c
I
c
data supplemented by archival data from Gaia eDR3 and Pan-STARRS. The stellar memberships are determined using a statistical method based on Gaia eDR3 kinematic data, and we found 204 members in SAI 44 while only 74 members are identified in SAI 45. The average distances to SAI 44 and SAI 45 are calculated to be 3670 ± 184 and 1668 ± 47 pc. The logarithmic age of the clusters are determined to be 8.82 ± 0.10 and 9.07 ± 0.10 yr for SAI 44 and SAI 45, respectively. The color–magnitude diagram of SAI 45 hosts an extended main-sequence turnoff (eMSTO). The apparent age spread is found to be similar to the apparent age spread predicted on the basis of the age spread and cluster age relation predicted by rotation models. This indicates that eMSTO is a stellar evolution rather than star formation phenomenon in SAI 45. We conclude that eMSTO in SAI 45 is mainly caused by the different rotation rates of stars as the SYCLIST synthetic population with different rotation rates was able to reproduce the observed eMSTO, and stars in the red part of the eMSTO were preferentially concentrated in the inner region, which again hints at different rotations being the reason for the extension in the upper MS. This finding supports the theory attributing the origin of eMSTO to the different rotations of eMSTO stars. The mass function slopes are obtained as −2.24 ± 0.66 and −2.58 ± 3.20 in the mass rages 2.426–0.990
M
⊙
and 2.167–1.202
M
⊙
for SAI 44 and SAI 45, respectively. SAI 44 exhibits the signature of mass segregation while we found weak evidence of mass segregation in SAI 45 possibly due to tidal stripping. The dynamical relaxation times of these clusters indicate that both clusters are in a dynamically relaxed state. Using the AD-diagram method, the apex coordinates are found to be (
69
.°
79
±
0
.°
11
, −
30
.°
82
±
0
.°
15
) for SAI 44 and (−
56
.°
22
±
0
.°
13
, −
56
.°
62
±
0
.°
13
) for SAI 45. The average space velocity components of the clusters SAI 44 and SAI 45 are calculated in units of km s
−1
as (−15.14 ± 3.90, −19.43 ± 4.41, −20.85 ± 4.57) and (28.13 ± 5.30, −9.78 ± 3.13, −19.59 ± 4.43), respectively.</description><identifier>ISSN: 0004-6256</identifier><identifier>ISSN: 1538-3881</identifier><identifier>EISSN: 1538-3881</identifier><identifier>DOI: 10.3847/1538-3881/ac0138</identifier><language>eng</language><publisher>Madison: The American Astronomical Society</publisher><subject>Age ; Astronomical models ; Astronomy ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; CCD photometry ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; Kinematics ; Open clusters ; Open star clusters ; Photometry ; RELAXATION ; ROTATION ; SEGREGATION ; SPACE ; Star & galaxy formation ; STAR EVOLUTION ; Star formation ; STARS ; Statistical methods ; Stellar evolution ; Stellar mass functions ; Stellar rotation ; VELOCITY</subject><ispartof>The Astronomical journal, 2021-08, Vol.162 (2), p.64</ispartof><rights>2021. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Aug 2021</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c378t-edb24caeb98cbc254865f45e7e6bae19b24c56fb1e0546c5dd6012173040c64b3</citedby><cites>FETCH-LOGICAL-c378t-edb24caeb98cbc254865f45e7e6bae19b24c56fb1e0546c5dd6012173040c64b3</cites><orcidid>0000-0001-8657-1573 ; 0000-0001-5119-8983 ; 0000-0001-5731-3057 ; 0000-0002-2298-4026</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/ac0138/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,777,781,882,27905,27906,38849,38871,53821,53848</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/ac0138$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://www.osti.gov/biblio/23159310$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Maurya, Jayanand</creatorcontrib><creatorcontrib>Joshi, Y. C.</creatorcontrib><creatorcontrib>Elsanhoury, W. H.</creatorcontrib><creatorcontrib>Sharma, Saurabh</creatorcontrib><title>Photometric and Kinematic Study of the Open Clusters SAI 44 and SAI 45</title><title>The Astronomical journal</title><addtitle>AJ</addtitle><addtitle>Astron. J</addtitle><description>We carry out a detailed photometric and kinematic study of the poorly studied sparse open clusters SAI 44 and SAI 45 using ground-based
BVR
c
I
c
data supplemented by archival data from Gaia eDR3 and Pan-STARRS. The stellar memberships are determined using a statistical method based on Gaia eDR3 kinematic data, and we found 204 members in SAI 44 while only 74 members are identified in SAI 45. The average distances to SAI 44 and SAI 45 are calculated to be 3670 ± 184 and 1668 ± 47 pc. The logarithmic age of the clusters are determined to be 8.82 ± 0.10 and 9.07 ± 0.10 yr for SAI 44 and SAI 45, respectively. The color–magnitude diagram of SAI 45 hosts an extended main-sequence turnoff (eMSTO). The apparent age spread is found to be similar to the apparent age spread predicted on the basis of the age spread and cluster age relation predicted by rotation models. This indicates that eMSTO is a stellar evolution rather than star formation phenomenon in SAI 45. We conclude that eMSTO in SAI 45 is mainly caused by the different rotation rates of stars as the SYCLIST synthetic population with different rotation rates was able to reproduce the observed eMSTO, and stars in the red part of the eMSTO were preferentially concentrated in the inner region, which again hints at different rotations being the reason for the extension in the upper MS. This finding supports the theory attributing the origin of eMSTO to the different rotations of eMSTO stars. The mass function slopes are obtained as −2.24 ± 0.66 and −2.58 ± 3.20 in the mass rages 2.426–0.990
M
⊙
and 2.167–1.202
M
⊙
for SAI 44 and SAI 45, respectively. SAI 44 exhibits the signature of mass segregation while we found weak evidence of mass segregation in SAI 45 possibly due to tidal stripping. The dynamical relaxation times of these clusters indicate that both clusters are in a dynamically relaxed state. Using the AD-diagram method, the apex coordinates are found to be (
69
.°
79
±
0
.°
11
, −
30
.°
82
±
0
.°
15
) for SAI 44 and (−
56
.°
22
±
0
.°
13
, −
56
.°
62
±
0
.°
13
) for SAI 45. The average space velocity components of the clusters SAI 44 and SAI 45 are calculated in units of km s
−1
as (−15.14 ± 3.90, −19.43 ± 4.41, −20.85 ± 4.57) and (28.13 ± 5.30, −9.78 ± 3.13, −19.59 ± 4.43), respectively.</description><subject>Age</subject><subject>Astronomical models</subject><subject>Astronomy</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>CCD photometry</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>Kinematics</subject><subject>Open clusters</subject><subject>Open star clusters</subject><subject>Photometry</subject><subject>RELAXATION</subject><subject>ROTATION</subject><subject>SEGREGATION</subject><subject>SPACE</subject><subject>Star & galaxy formation</subject><subject>STAR EVOLUTION</subject><subject>Star formation</subject><subject>STARS</subject><subject>Statistical methods</subject><subject>Stellar evolution</subject><subject>Stellar mass functions</subject><subject>Stellar rotation</subject><subject>VELOCITY</subject><issn>0004-6256</issn><issn>1538-3881</issn><issn>1538-3881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNp1kDtPwzAUhS0EEqWwM1piJXAdP-KOVUWholKRCrOVODdqqjYOtjv035M0iE5M9_Wdo6tDyD2DJ65F9swk1wnXmj3nFhjXF2T0t7okIwAQiUqluiY3IWwBGNMgRmT-sXHR7TH62tK8Kel73eA-j920jofySF1F4wbpqsWGznaHENEHup4uqBAn_tTKW3JV5buAd791TL7mL5-zt2S5el3MpsvE8kzHBMsiFTbHYqJtYVMptJKVkJihKnJkk_4qVVUwBCmUlWWpgKUs4yDAKlHwMXkYfF2ItQm2jmg31jUN2mhSzuSEMzhTrXffBwzRbN3BN91jJpWS81QJLjoKBsp6F4LHyrS-3uf-aBiYPlPTB2j6AM2QaSd5HCS1a8-e_-I_FlxzpA</recordid><startdate>20210801</startdate><enddate>20210801</enddate><creator>Maurya, Jayanand</creator><creator>Joshi, Y. C.</creator><creator>Elsanhoury, W. H.</creator><creator>Sharma, Saurabh</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0001-8657-1573</orcidid><orcidid>https://orcid.org/0000-0001-5119-8983</orcidid><orcidid>https://orcid.org/0000-0001-5731-3057</orcidid><orcidid>https://orcid.org/0000-0002-2298-4026</orcidid></search><sort><creationdate>20210801</creationdate><title>Photometric and Kinematic Study of the Open Clusters SAI 44 and SAI 45</title><author>Maurya, Jayanand ; Joshi, Y. C. ; Elsanhoury, W. H. ; Sharma, Saurabh</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c378t-edb24caeb98cbc254865f45e7e6bae19b24c56fb1e0546c5dd6012173040c64b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Age</topic><topic>Astronomical models</topic><topic>Astronomy</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>CCD photometry</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>Kinematics</topic><topic>Open clusters</topic><topic>Open star clusters</topic><topic>Photometry</topic><topic>RELAXATION</topic><topic>ROTATION</topic><topic>SEGREGATION</topic><topic>SPACE</topic><topic>Star & galaxy formation</topic><topic>STAR EVOLUTION</topic><topic>Star formation</topic><topic>STARS</topic><topic>Statistical methods</topic><topic>Stellar evolution</topic><topic>Stellar mass functions</topic><topic>Stellar rotation</topic><topic>VELOCITY</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Maurya, Jayanand</creatorcontrib><creatorcontrib>Joshi, Y. C.</creatorcontrib><creatorcontrib>Elsanhoury, W. H.</creatorcontrib><creatorcontrib>Sharma, Saurabh</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>The Astronomical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Maurya, Jayanand</au><au>Joshi, Y. C.</au><au>Elsanhoury, W. H.</au><au>Sharma, Saurabh</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Photometric and Kinematic Study of the Open Clusters SAI 44 and SAI 45</atitle><jtitle>The Astronomical journal</jtitle><stitle>AJ</stitle><addtitle>Astron. J</addtitle><date>2021-08-01</date><risdate>2021</risdate><volume>162</volume><issue>2</issue><spage>64</spage><pages>64-</pages><issn>0004-6256</issn><issn>1538-3881</issn><eissn>1538-3881</eissn><abstract>We carry out a detailed photometric and kinematic study of the poorly studied sparse open clusters SAI 44 and SAI 45 using ground-based
BVR
c
I
c
data supplemented by archival data from Gaia eDR3 and Pan-STARRS. The stellar memberships are determined using a statistical method based on Gaia eDR3 kinematic data, and we found 204 members in SAI 44 while only 74 members are identified in SAI 45. The average distances to SAI 44 and SAI 45 are calculated to be 3670 ± 184 and 1668 ± 47 pc. The logarithmic age of the clusters are determined to be 8.82 ± 0.10 and 9.07 ± 0.10 yr for SAI 44 and SAI 45, respectively. The color–magnitude diagram of SAI 45 hosts an extended main-sequence turnoff (eMSTO). The apparent age spread is found to be similar to the apparent age spread predicted on the basis of the age spread and cluster age relation predicted by rotation models. This indicates that eMSTO is a stellar evolution rather than star formation phenomenon in SAI 45. We conclude that eMSTO in SAI 45 is mainly caused by the different rotation rates of stars as the SYCLIST synthetic population with different rotation rates was able to reproduce the observed eMSTO, and stars in the red part of the eMSTO were preferentially concentrated in the inner region, which again hints at different rotations being the reason for the extension in the upper MS. This finding supports the theory attributing the origin of eMSTO to the different rotations of eMSTO stars. The mass function slopes are obtained as −2.24 ± 0.66 and −2.58 ± 3.20 in the mass rages 2.426–0.990
M
⊙
and 2.167–1.202
M
⊙
for SAI 44 and SAI 45, respectively. SAI 44 exhibits the signature of mass segregation while we found weak evidence of mass segregation in SAI 45 possibly due to tidal stripping. The dynamical relaxation times of these clusters indicate that both clusters are in a dynamically relaxed state. Using the AD-diagram method, the apex coordinates are found to be (
69
.°
79
±
0
.°
11
, −
30
.°
82
±
0
.°
15
) for SAI 44 and (−
56
.°
22
±
0
.°
13
, −
56
.°
62
±
0
.°
13
) for SAI 45. The average space velocity components of the clusters SAI 44 and SAI 45 are calculated in units of km s
−1
as (−15.14 ± 3.90, −19.43 ± 4.41, −20.85 ± 4.57) and (28.13 ± 5.30, −9.78 ± 3.13, −19.59 ± 4.43), respectively.</abstract><cop>Madison</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-3881/ac0138</doi><tpages>14</tpages><orcidid>https://orcid.org/0000-0001-8657-1573</orcidid><orcidid>https://orcid.org/0000-0001-5119-8983</orcidid><orcidid>https://orcid.org/0000-0001-5731-3057</orcidid><orcidid>https://orcid.org/0000-0002-2298-4026</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | The Astronomical journal, 2021-08, Vol.162 (2), p.64 |
| issn | 0004-6256 1538-3881 1538-3881 |
| language | eng |
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| source | IOP Publishing Free Content |
| subjects | Age Astronomical models Astronomy ASTROPHYSICS, COSMOLOGY AND ASTRONOMY CCD photometry CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS Kinematics Open clusters Open star clusters Photometry RELAXATION ROTATION SEGREGATION SPACE Star & galaxy formation STAR EVOLUTION Star formation STARS Statistical methods Stellar evolution Stellar mass functions Stellar rotation VELOCITY |
| title | Photometric and Kinematic Study of the Open Clusters SAI 44 and SAI 45 |
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