Gaia23bab: A New EXor
On 2023 March 6, the Gaia telescope alerted a 2 mag burst from Gaia23bab, a young stellar object in the Galactic plane. We observed Gaia23bab with the Large Binocular Telescope obtaining optical and near-infrared spectra close in time to the peak of the burst, and collected all public multiband phot...
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| Veröffentlicht in: | The Astrophysical journal 2024-05, Vol.967 (1), p.41 |
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| creator | Giannini, T. Schisano, E. Nisini, B. Ábrahám, P. Antoniucci, S. Biazzo, K. Cruz-Sáenz de Miera, F. Fiorellino, E. Gangi, M. Kóspál, A. Kuhn, M. Marini, E. Nagy, Z. Paris, D. |
| description | On 2023 March 6, the Gaia telescope alerted a 2 mag burst from Gaia23bab, a young stellar object in the Galactic plane. We observed Gaia23bab with the Large Binocular Telescope obtaining optical and near-infrared spectra close in time to the peak of the burst, and collected all public multiband photometry to reconstruct the historical light curve. The latter shows three bursts in 10 years (2013, 2017, and 2023), whose duration and amplitude are typical of EXor variables. We estimate that, due to the bursts, the mass accumulated on the star is about twice greater than if the source had remained quiescent for the same period of time. Photometric analysis indicates that Gaia23bab is a class II source with age ≲1 Myr, spectral type G3−K0, stellar luminosity ∼4.0
L
⊙
, and mass ∼1.6
M
⊙
. The optical/near-infrared spectrum is rich in emission lines. From the analysis of these lines we measured an accretion luminosity and mass accretion rate (
L
acc
burst
∼ 3.7
L
⊙
,
M
̇
acc
burst
∼ 2.0 × 10
−7
M
⊙
yr
−1
) consistent with those of EXors. More generally, we derived the relationships between accretion and stellar parameters in a sample of EXors. We find that, when in burst, the accretion parameters become almost independent of the stellar parameters and that EXors, even in quiescence, are more efficient than classical T Tauri stars in assembling mass. |
| doi_str_mv | 10.3847/1538-4357/ad39e2 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_iop_j</sourceid><recordid>TN_cdi_iop_journals_10_3847_1538_4357_ad39e2</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><doaj_id>oai_doaj_org_article_1006606c54e444d19f6215c561a4b763</doaj_id><sourcerecordid>3055937065</sourcerecordid><originalsourceid>FETCH-LOGICAL-c432t-213c8efbf3efca7f2e086369b0b9a7a3ae8bef28424b833b9f8cf784b05c27c23</originalsourceid><addsrcrecordid>eNp1kE1LAzEQhoMoWKtHwWNBL4Jrk0w-vZVSW6HoRaG3kGQT3VLdNdsq_nt3XakIehrm5ZkH5kXohOBLUEwOCQeVMeByaHPQge6g3jbaRT2MMcsEyMU-OqjrZbtSrXvoeGoLS8FZdzUYDW7D-2CyKNMh2ot2VYej79lHD9eT-_Esm99Nb8ajeeYZ0HVGCXgVoosQorcy0oCVAKEddtpKCzYoFyJVjDKnAJyOykepmMPcU-kp9NFN581LuzRVKp5t-jClLcxXUKZHY9O68KtgCMZCYOE5C4yxnOgoKOGeC2KZkwIa13nnerKrX6rZaG7aDDNFsJTijTTsacdWqXzdhHptluUmvTSvGsCca5BY8IbCHeVTWdcpxK2WYNOWbtqGTduw6UpvTs66k6Ksfpy2WhotGtwwYqo8NtjFH9i_1k-eLIm0</addsrcrecordid><sourcetype>Open Website</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>3055937065</pqid></control><display><type>article</type><title>Gaia23bab: A New EXor</title><source>IOP Publishing Free Content</source><source>DOAJ Directory of Open Access Journals</source><source>Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals</source><source>Alma/SFX Local Collection</source><creator>Giannini, T. ; Schisano, E. ; Nisini, B. ; Ábrahám, P. ; Antoniucci, S. ; Biazzo, K. ; Cruz-Sáenz de Miera, F. ; Fiorellino, E. ; Gangi, M. ; Kóspál, A. ; Kuhn, M. ; Marini, E. ; Nagy, Z. ; Paris, D.</creator><creatorcontrib>Giannini, T. ; Schisano, E. ; Nisini, B. ; Ábrahám, P. ; Antoniucci, S. ; Biazzo, K. ; Cruz-Sáenz de Miera, F. ; Fiorellino, E. ; Gangi, M. ; Kóspál, A. ; Kuhn, M. ; Marini, E. ; Nagy, Z. ; Paris, D.</creatorcontrib><description>On 2023 March 6, the Gaia telescope alerted a 2 mag burst from Gaia23bab, a young stellar object in the Galactic plane. We observed Gaia23bab with the Large Binocular Telescope obtaining optical and near-infrared spectra close in time to the peak of the burst, and collected all public multiband photometry to reconstruct the historical light curve. The latter shows three bursts in 10 years (2013, 2017, and 2023), whose duration and amplitude are typical of EXor variables. We estimate that, due to the bursts, the mass accumulated on the star is about twice greater than if the source had remained quiescent for the same period of time. Photometric analysis indicates that Gaia23bab is a class II source with age ≲1 Myr, spectral type G3−K0, stellar luminosity ∼4.0
L
⊙
, and mass ∼1.6
M
⊙
. The optical/near-infrared spectrum is rich in emission lines. From the analysis of these lines we measured an accretion luminosity and mass accretion rate (
L
acc
burst
∼ 3.7
L
⊙
,
M
̇
acc
burst
∼ 2.0 × 10
−7
M
⊙
yr
−1
) consistent with those of EXors. More generally, we derived the relationships between accretion and stellar parameters in a sample of EXors. We find that, when in burst, the accretion parameters become almost independent of the stellar parameters and that EXors, even in quiescence, are more efficient than classical T Tauri stars in assembling mass.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ad39e2</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Bursts ; Emission lines ; Eruptive variable stars ; Infrared analysis ; Infrared spectra ; Light curve ; Luminosity ; Near infrared radiation ; Parameters ; Photometry ; Physics ; Pre-main sequence stars ; Star formation ; Stellar accretion ; Stellar luminosity ; T Tauri stars</subject><ispartof>The Astrophysical journal, 2024-05, Vol.967 (1), p.41</ispartof><rights>2024. The Author(s). Published by the American Astronomical Society.</rights><rights>2024. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>Attribution</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c432t-213c8efbf3efca7f2e086369b0b9a7a3ae8bef28424b833b9f8cf784b05c27c23</cites><orcidid>0000-0002-0666-3847 ; 0000-0002-7035-8513 ; 0000-0002-8364-7795 ; 0000-0002-7409-8114 ; 0000-0002-9190-0113 ; 0000-0001-6015-646X ; 0000-0002-5261-6216 ; 0000-0002-3632-1194 ; 0000-0002-1892-2180 ; 0000-0002-6894-1267 ; 0000-0001-7157-6275 ; 0000-0003-1560-3958 ; 0000-0002-0631-7514 ; 0000-0002-4283-2185</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ad39e2/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>230,314,776,780,860,881,2096,27901,27902,38867,53842</link.rule.ids><backlink>$$Uhttps://hal.science/hal-04810776$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Giannini, T.</creatorcontrib><creatorcontrib>Schisano, E.</creatorcontrib><creatorcontrib>Nisini, B.</creatorcontrib><creatorcontrib>Ábrahám, P.</creatorcontrib><creatorcontrib>Antoniucci, S.</creatorcontrib><creatorcontrib>Biazzo, K.</creatorcontrib><creatorcontrib>Cruz-Sáenz de Miera, F.</creatorcontrib><creatorcontrib>Fiorellino, E.</creatorcontrib><creatorcontrib>Gangi, M.</creatorcontrib><creatorcontrib>Kóspál, A.</creatorcontrib><creatorcontrib>Kuhn, M.</creatorcontrib><creatorcontrib>Marini, E.</creatorcontrib><creatorcontrib>Nagy, Z.</creatorcontrib><creatorcontrib>Paris, D.</creatorcontrib><title>Gaia23bab: A New EXor</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>On 2023 March 6, the Gaia telescope alerted a 2 mag burst from Gaia23bab, a young stellar object in the Galactic plane. We observed Gaia23bab with the Large Binocular Telescope obtaining optical and near-infrared spectra close in time to the peak of the burst, and collected all public multiband photometry to reconstruct the historical light curve. The latter shows three bursts in 10 years (2013, 2017, and 2023), whose duration and amplitude are typical of EXor variables. We estimate that, due to the bursts, the mass accumulated on the star is about twice greater than if the source had remained quiescent for the same period of time. Photometric analysis indicates that Gaia23bab is a class II source with age ≲1 Myr, spectral type G3−K0, stellar luminosity ∼4.0
L
⊙
, and mass ∼1.6
M
⊙
. The optical/near-infrared spectrum is rich in emission lines. From the analysis of these lines we measured an accretion luminosity and mass accretion rate (
L
acc
burst
∼ 3.7
L
⊙
,
M
̇
acc
burst
∼ 2.0 × 10
−7
M
⊙
yr
−1
) consistent with those of EXors. More generally, we derived the relationships between accretion and stellar parameters in a sample of EXors. We find that, when in burst, the accretion parameters become almost independent of the stellar parameters and that EXors, even in quiescence, are more efficient than classical T Tauri stars in assembling mass.</description><subject>Astrophysics</subject><subject>Bursts</subject><subject>Emission lines</subject><subject>Eruptive variable stars</subject><subject>Infrared analysis</subject><subject>Infrared spectra</subject><subject>Light curve</subject><subject>Luminosity</subject><subject>Near infrared radiation</subject><subject>Parameters</subject><subject>Photometry</subject><subject>Physics</subject><subject>Pre-main sequence stars</subject><subject>Star formation</subject><subject>Stellar accretion</subject><subject>Stellar luminosity</subject><subject>T Tauri stars</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp1kE1LAzEQhoMoWKtHwWNBL4Jrk0w-vZVSW6HoRaG3kGQT3VLdNdsq_nt3XakIehrm5ZkH5kXohOBLUEwOCQeVMeByaHPQge6g3jbaRT2MMcsEyMU-OqjrZbtSrXvoeGoLS8FZdzUYDW7D-2CyKNMh2ot2VYej79lHD9eT-_Esm99Nb8ajeeYZ0HVGCXgVoosQorcy0oCVAKEddtpKCzYoFyJVjDKnAJyOykepmMPcU-kp9NFN581LuzRVKp5t-jClLcxXUKZHY9O68KtgCMZCYOE5C4yxnOgoKOGeC2KZkwIa13nnerKrX6rZaG7aDDNFsJTijTTsacdWqXzdhHptluUmvTSvGsCca5BY8IbCHeVTWdcpxK2WYNOWbtqGTduw6UpvTs66k6Ksfpy2WhotGtwwYqo8NtjFH9i_1k-eLIm0</recordid><startdate>20240501</startdate><enddate>20240501</enddate><creator>Giannini, T.</creator><creator>Schisano, E.</creator><creator>Nisini, B.</creator><creator>Ábrahám, P.</creator><creator>Antoniucci, S.</creator><creator>Biazzo, K.</creator><creator>Cruz-Sáenz de Miera, F.</creator><creator>Fiorellino, E.</creator><creator>Gangi, M.</creator><creator>Kóspál, A.</creator><creator>Kuhn, M.</creator><creator>Marini, E.</creator><creator>Nagy, Z.</creator><creator>Paris, D.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><general>American Astronomical Society</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>1XC</scope><scope>VOOES</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0002-0666-3847</orcidid><orcidid>https://orcid.org/0000-0002-7035-8513</orcidid><orcidid>https://orcid.org/0000-0002-8364-7795</orcidid><orcidid>https://orcid.org/0000-0002-7409-8114</orcidid><orcidid>https://orcid.org/0000-0002-9190-0113</orcidid><orcidid>https://orcid.org/0000-0001-6015-646X</orcidid><orcidid>https://orcid.org/0000-0002-5261-6216</orcidid><orcidid>https://orcid.org/0000-0002-3632-1194</orcidid><orcidid>https://orcid.org/0000-0002-1892-2180</orcidid><orcidid>https://orcid.org/0000-0002-6894-1267</orcidid><orcidid>https://orcid.org/0000-0001-7157-6275</orcidid><orcidid>https://orcid.org/0000-0003-1560-3958</orcidid><orcidid>https://orcid.org/0000-0002-0631-7514</orcidid><orcidid>https://orcid.org/0000-0002-4283-2185</orcidid></search><sort><creationdate>20240501</creationdate><title>Gaia23bab: A New EXor</title><author>Giannini, T. ; 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J</addtitle><date>2024-05-01</date><risdate>2024</risdate><volume>967</volume><issue>1</issue><spage>41</spage><pages>41-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>On 2023 March 6, the Gaia telescope alerted a 2 mag burst from Gaia23bab, a young stellar object in the Galactic plane. We observed Gaia23bab with the Large Binocular Telescope obtaining optical and near-infrared spectra close in time to the peak of the burst, and collected all public multiband photometry to reconstruct the historical light curve. The latter shows three bursts in 10 years (2013, 2017, and 2023), whose duration and amplitude are typical of EXor variables. We estimate that, due to the bursts, the mass accumulated on the star is about twice greater than if the source had remained quiescent for the same period of time. Photometric analysis indicates that Gaia23bab is a class II source with age ≲1 Myr, spectral type G3−K0, stellar luminosity ∼4.0
L
⊙
, and mass ∼1.6
M
⊙
. The optical/near-infrared spectrum is rich in emission lines. From the analysis of these lines we measured an accretion luminosity and mass accretion rate (
L
acc
burst
∼ 3.7
L
⊙
,
M
̇
acc
burst
∼ 2.0 × 10
−7
M
⊙
yr
−1
) consistent with those of EXors. More generally, we derived the relationships between accretion and stellar parameters in a sample of EXors. We find that, when in burst, the accretion parameters become almost independent of the stellar parameters and that EXors, even in quiescence, are more efficient than classical T Tauri stars in assembling mass.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ad39e2</doi><tpages>12</tpages><orcidid>https://orcid.org/0000-0002-0666-3847</orcidid><orcidid>https://orcid.org/0000-0002-7035-8513</orcidid><orcidid>https://orcid.org/0000-0002-8364-7795</orcidid><orcidid>https://orcid.org/0000-0002-7409-8114</orcidid><orcidid>https://orcid.org/0000-0002-9190-0113</orcidid><orcidid>https://orcid.org/0000-0001-6015-646X</orcidid><orcidid>https://orcid.org/0000-0002-5261-6216</orcidid><orcidid>https://orcid.org/0000-0002-3632-1194</orcidid><orcidid>https://orcid.org/0000-0002-1892-2180</orcidid><orcidid>https://orcid.org/0000-0002-6894-1267</orcidid><orcidid>https://orcid.org/0000-0001-7157-6275</orcidid><orcidid>https://orcid.org/0000-0003-1560-3958</orcidid><orcidid>https://orcid.org/0000-0002-0631-7514</orcidid><orcidid>https://orcid.org/0000-0002-4283-2185</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2024-05, Vol.967 (1), p.41 |
| issn | 0004-637X 1538-4357 |
| language | eng |
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| source | IOP Publishing Free Content; DOAJ Directory of Open Access Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; Alma/SFX Local Collection |
| subjects | Astrophysics Bursts Emission lines Eruptive variable stars Infrared analysis Infrared spectra Light curve Luminosity Near infrared radiation Parameters Photometry Physics Pre-main sequence stars Star formation Stellar accretion Stellar luminosity T Tauri stars |
| title | Gaia23bab: A New EXor |
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