Teutsch 76: A deep near-infrared study
Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data r...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Sharma, Saurabh [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2023 |
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| Schlagwörter: |
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| Anmerkung: |
© Indian Academy of Sciences 2023 |
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| Übergeordnetes Werk: |
Enthalten in: Journal of astrophysics and astronomy - Bangalore : Springer India, 1980, 44(2023), 1 vom: 13. Mai |
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| Übergeordnetes Werk: |
volume:44 ; year:2023 ; number:1 ; day:13 ; month:05 |
| Links: |
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| DOI / URN: |
10.1007/s12036-023-09936-w |
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SPR05242572X |
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| 100 | 1 | |a Sharma, Saurabh |e verfasserin |0 (orcid)0000-0001-5731-3057 |4 aut | |
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| 520 | |a Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. | ||
| 650 | 4 | |a Star cluster |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a star formation |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a stellar evolution |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Dewangan, Lokesh |4 aut | |
| 700 | 1 | |a Panwar, Neelam |4 aut | |
| 700 | 1 | |a Kaur, Harmeen |4 aut | |
| 700 | 1 | |a Ojha, Devendra K. |4 aut | |
| 700 | 1 | |a Yadav, Ramkesh |4 aut | |
| 700 | 1 | |a Verma, Aayushi |4 aut | |
| 700 | 1 | |a Baug, Tapas |4 aut | |
| 700 | 1 | |a Sinha, Tirthendu |4 aut | |
| 700 | 1 | |a Pandey, Rakesh |4 aut | |
| 700 | 1 | |a Ghosh, Arpan |4 aut | |
| 700 | 1 | |a Chand, Tarak |4 aut | |
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| 773 | 1 | 8 | |g volume:44 |g year:2023 |g number:1 |g day:13 |g month:05 |
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10.1007/s12036-023-09936-w doi (DE-627)SPR05242572X (SPR)s12036-023-09936-w-e DE-627 ger DE-627 rakwb eng Sharma, Saurabh verfasserin (orcid)0000-0001-5731-3057 aut Teutsch 76: A deep near-infrared study 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2023 Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. Star cluster (dpeaa)DE-He213 star formation (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Dewangan, Lokesh aut Panwar, Neelam aut Kaur, Harmeen aut Ojha, Devendra K. aut Yadav, Ramkesh aut Verma, Aayushi aut Baug, Tapas aut Sinha, Tirthendu aut Pandey, Rakesh aut Ghosh, Arpan aut Chand, Tarak aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 44(2023), 1 vom: 13. Mai (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:44 year:2023 number:1 day:13 month:05 https://dx.doi.org/10.1007/s12036-023-09936-w lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 44 2023 1 13 05 |
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10.1007/s12036-023-09936-w doi (DE-627)SPR05242572X (SPR)s12036-023-09936-w-e DE-627 ger DE-627 rakwb eng Sharma, Saurabh verfasserin (orcid)0000-0001-5731-3057 aut Teutsch 76: A deep near-infrared study 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2023 Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. Star cluster (dpeaa)DE-He213 star formation (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Dewangan, Lokesh aut Panwar, Neelam aut Kaur, Harmeen aut Ojha, Devendra K. aut Yadav, Ramkesh aut Verma, Aayushi aut Baug, Tapas aut Sinha, Tirthendu aut Pandey, Rakesh aut Ghosh, Arpan aut Chand, Tarak aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 44(2023), 1 vom: 13. Mai (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:44 year:2023 number:1 day:13 month:05 https://dx.doi.org/10.1007/s12036-023-09936-w lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 44 2023 1 13 05 |
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10.1007/s12036-023-09936-w doi (DE-627)SPR05242572X (SPR)s12036-023-09936-w-e DE-627 ger DE-627 rakwb eng Sharma, Saurabh verfasserin (orcid)0000-0001-5731-3057 aut Teutsch 76: A deep near-infrared study 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2023 Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. Star cluster (dpeaa)DE-He213 star formation (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Dewangan, Lokesh aut Panwar, Neelam aut Kaur, Harmeen aut Ojha, Devendra K. aut Yadav, Ramkesh aut Verma, Aayushi aut Baug, Tapas aut Sinha, Tirthendu aut Pandey, Rakesh aut Ghosh, Arpan aut Chand, Tarak aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 44(2023), 1 vom: 13. Mai (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:44 year:2023 number:1 day:13 month:05 https://dx.doi.org/10.1007/s12036-023-09936-w lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 44 2023 1 13 05 |
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10.1007/s12036-023-09936-w doi (DE-627)SPR05242572X (SPR)s12036-023-09936-w-e DE-627 ger DE-627 rakwb eng Sharma, Saurabh verfasserin (orcid)0000-0001-5731-3057 aut Teutsch 76: A deep near-infrared study 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2023 Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. Star cluster (dpeaa)DE-He213 star formation (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Dewangan, Lokesh aut Panwar, Neelam aut Kaur, Harmeen aut Ojha, Devendra K. aut Yadav, Ramkesh aut Verma, Aayushi aut Baug, Tapas aut Sinha, Tirthendu aut Pandey, Rakesh aut Ghosh, Arpan aut Chand, Tarak aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 44(2023), 1 vom: 13. Mai (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:44 year:2023 number:1 day:13 month:05 https://dx.doi.org/10.1007/s12036-023-09936-w lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 44 2023 1 13 05 |
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10.1007/s12036-023-09936-w doi (DE-627)SPR05242572X (SPR)s12036-023-09936-w-e DE-627 ger DE-627 rakwb eng Sharma, Saurabh verfasserin (orcid)0000-0001-5731-3057 aut Teutsch 76: A deep near-infrared study 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2023 Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. Star cluster (dpeaa)DE-He213 star formation (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Dewangan, Lokesh aut Panwar, Neelam aut Kaur, Harmeen aut Ojha, Devendra K. aut Yadav, Ramkesh aut Verma, Aayushi aut Baug, Tapas aut Sinha, Tirthendu aut Pandey, Rakesh aut Ghosh, Arpan aut Chand, Tarak aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 44(2023), 1 vom: 13. Mai (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:44 year:2023 number:1 day:13 month:05 https://dx.doi.org/10.1007/s12036-023-09936-w lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 44 2023 1 13 05 |
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Sharma, Saurabh @@aut@@ Dewangan, Lokesh @@aut@@ Panwar, Neelam @@aut@@ Kaur, Harmeen @@aut@@ Ojha, Devendra K. @@aut@@ Yadav, Ramkesh @@aut@@ Verma, Aayushi @@aut@@ Baug, Tapas @@aut@@ Sinha, Tirthendu @@aut@@ Pandey, Rakesh @@aut@@ Ghosh, Arpan @@aut@@ Chand, Tarak @@aut@@ |
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We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). 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Teutsch 76: A deep near-infrared study Star cluster (dpeaa)DE-He213 star formation (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 |
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Sharma, Saurabh Dewangan, Lokesh Panwar, Neelam Kaur, Harmeen Ojha, Devendra K. Yadav, Ramkesh Verma, Aayushi Baug, Tapas Sinha, Tirthendu Pandey, Rakesh Ghosh, Arpan Chand, Tarak |
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Teutsch 76: A deep near-infrared study |
| abstract |
Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. © Indian Academy of Sciences 2023 |
| abstractGer |
Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. © Indian Academy of Sciences 2023 |
| abstract_unstemmed |
Abstract We have performed a detailed analysis on the Teutsch 76 (T76) open cluster using the deep near-infrared (NIR) observations taken with the TANSPEC instrument mounted on the 3.6m Devasthal optical telescope along with the recently available high quality proper motion data from the Gaia data release 3 and deep photometric data from Pan-STARRS1 survey. We have found that the T76 cluster is having a central density concentration with circular morphology, probably due to the star-formation processes. The radius of the T76 cluster is found to be 45%$^{\prime \prime }%$ (1.24 pc) and 28 stars within this radius were marked as highly probable cluster members. We have found that the cluster is located at a distance of %$5.7\pm 1.0%$ kpc and is having an age of %$50\pm 10%$ Myr. The mass function slope (%$\Gamma %$) in the cluster region in the mass range of %$\sim %%%$0.75<M/M_\odot <5.8%$ is estimated as %$-1.3\pm 0.2%$, which is similar to the value of −1.35 given by Salpeter (1955). The cluster is not showing any signatures of mass-segregation and is currently undergoing dynamical relaxation. © Indian Academy of Sciences 2023 |
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| container_issue |
1 |
| title_short |
Teutsch 76: A deep near-infrared study |
| url |
https://dx.doi.org/10.1007/s12036-023-09936-w |
| remote_bool |
true |
| author2 |
Dewangan, Lokesh Panwar, Neelam Kaur, Harmeen Ojha, Devendra K. Yadav, Ramkesh Verma, Aayushi Baug, Tapas Sinha, Tirthendu Pandey, Rakesh Ghosh, Arpan Chand, Tarak |
| author2Str |
Dewangan, Lokesh Panwar, Neelam Kaur, Harmeen Ojha, Devendra K. Yadav, Ramkesh Verma, Aayushi Baug, Tapas Sinha, Tirthendu Pandey, Rakesh Ghosh, Arpan Chand, Tarak |
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| doi_str |
10.1007/s12036-023-09936-w |
| up_date |
2024-07-04T02:45:40.443Z |
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1803614830405353473 |
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| score |
7.39956 |