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A stellar dynamical mass measurement of an inactive black hole at redshift 2.

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Title: A stellar dynamical mass measurement of an inactive black hole at redshift 2.
Authors: Newman, Andrew B. (AUTHOR), Gu, Meng (AUTHOR), Belli, Sirio (AUTHOR), Ellis, Richard S. (AUTHOR), Gangula, Sai (AUTHOR), Greene, Jenny E. (AUTHOR), Walsh, Jonelle L. (AUTHOR), Suyu, Sherry H. (AUTHOR), Ertl, Sebastian (AUTHOR), Caminha, Gabriel (AUTHOR), Granata, Giovanni (AUTHOR), Grillo, Claudio (AUTHOR), Schuldt, Stefan (AUTHOR), Barone, Tania M. (AUTHOR), Bird, Simeon (AUTHOR), Glazebrook, Karl (AUTHOR), Jafariyazani, Marziye (AUTHOR), Kriek, Mariska (AUTHOR), Matthews, Allison (AUTHOR), Morishita, Takahiro (AUTHOR)
Source: Science. 6/4/2026, Vol. 392 Issue 6802, p1065-1068. 4p.
Subjects: Stellar dynamics, Gravitational lenses, Galactic evolution, Supermassive black holes, Galactic redshift, Space telescopes
Abstract: Supermassive black holes and their host galaxies grow together over time, producing correlations between the black hole mass and various galaxy properties. Determining the evolution of these correlations requires precise measurements of the masses of distant black holes. We observed the gravitationally lensed quiescent galaxy MRG-M0138 at redshift 1.95 using James Webb Space Telescope integral field spectroscopy to spatially resolve the kinematics of stars within the black hole's sphere of influence. By using a foreground lens model and fitting stellar dynamical models, we determined the mass of its inactive black hole to be M • = 6.0 − 1.7 + 2.1 × 10 9 solar masses. Comparing this measurement to local galaxies, we found that M • is higher than expected given the galaxy's bulge mass but consistent with the correlation of M • with stellar velocity dispersion. Editor's summary: Most galaxies contain a supermassive black hole at their center. The black hole mass can be determined from stellar kinematics, which requires a high spatial resolution that is usually only available for nearby targets. For more distant galaxies, the black hole mass must be inferred indirectly using empirical scaling relations, but it is unclear whether those are valid beyond the local Universe. Newman et al. took advantage of a gravitational lens that magnifies a distant galaxy. This approach provides sufficient spatial resolution to model the stellar kinematics and determine the black hole mass. Its value is consistent with one local scaling relation but inconsistent with another. —Keith T. Smith [ABSTRACT FROM AUTHOR]
Copyright of Science is the property of American Association for the Advancement of Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: Psychology and Behavioral Sciences Collection
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  Data: A stellar dynamical mass measurement of an inactive black hole at redshift 2.
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  Data: <searchLink fieldCode="AR" term="%22Newman%2C+Andrew+B%2E%22">Newman, Andrew B.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Gu%2C+Meng%22">Gu, Meng</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Belli%2C+Sirio%22">Belli, Sirio</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Ellis%2C+Richard+S%2E%22">Ellis, Richard S.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Gangula%2C+Sai%22">Gangula, Sai</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Greene%2C+Jenny+E%2E%22">Greene, Jenny E.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Walsh%2C+Jonelle+L%2E%22">Walsh, Jonelle L.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Suyu%2C+Sherry+H%2E%22">Suyu, Sherry H.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Ertl%2C+Sebastian%22">Ertl, Sebastian</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Caminha%2C+Gabriel%22">Caminha, Gabriel</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Granata%2C+Giovanni%22">Granata, Giovanni</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Grillo%2C+Claudio%22">Grillo, Claudio</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Schuldt%2C+Stefan%22">Schuldt, Stefan</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Barone%2C+Tania+M%2E%22">Barone, Tania M.</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Bird%2C+Simeon%22">Bird, Simeon</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Glazebrook%2C+Karl%22">Glazebrook, Karl</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Jafariyazani%2C+Marziye%22">Jafariyazani, Marziye</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Kriek%2C+Mariska%22">Kriek, Mariska</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Matthews%2C+Allison%22">Matthews, Allison</searchLink> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Morishita%2C+Takahiro%22">Morishita, Takahiro</searchLink> (AUTHOR)
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  Data: <searchLink fieldCode="JN" term="%22Science%22">Science</searchLink>. 6/4/2026, Vol. 392 Issue 6802, p1065-1068. 4p.
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  Data: <searchLink fieldCode="DE" term="%22Stellar+dynamics%22">Stellar dynamics</searchLink><br /><searchLink fieldCode="DE" term="%22Gravitational+lenses%22">Gravitational lenses</searchLink><br /><searchLink fieldCode="DE" term="%22Galactic+evolution%22">Galactic evolution</searchLink><br /><searchLink fieldCode="DE" term="%22Supermassive+black+holes%22">Supermassive black holes</searchLink><br /><searchLink fieldCode="DE" term="%22Galactic+redshift%22">Galactic redshift</searchLink><br /><searchLink fieldCode="DE" term="%22Space+telescopes%22">Space telescopes</searchLink>
– Name: Abstract
  Label: Abstract
  Group: Ab
  Data: Supermassive black holes and their host galaxies grow together over time, producing correlations between the black hole mass and various galaxy properties. Determining the evolution of these correlations requires precise measurements of the masses of distant black holes. We observed the gravitationally lensed quiescent galaxy MRG-M0138 at redshift 1.95 using James Webb Space Telescope integral field spectroscopy to spatially resolve the kinematics of stars within the black hole's sphere of influence. By using a foreground lens model and fitting stellar dynamical models, we determined the mass of its inactive black hole to be M • = 6.0 − 1.7 + 2.1 × 10 9 solar masses. Comparing this measurement to local galaxies, we found that M • is higher than expected given the galaxy's bulge mass but consistent with the correlation of M • with stellar velocity dispersion. Editor's summary: Most galaxies contain a supermassive black hole at their center. The black hole mass can be determined from stellar kinematics, which requires a high spatial resolution that is usually only available for nearby targets. For more distant galaxies, the black hole mass must be inferred indirectly using empirical scaling relations, but it is unclear whether those are valid beyond the local Universe. Newman et al. took advantage of a gravitational lens that magnifies a distant galaxy. This approach provides sufficient spatial resolution to model the stellar kinematics and determine the black hole mass. Its value is consistent with one local scaling relation but inconsistent with another. —Keith T. Smith [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
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  Data: <i>Copyright of Science is the property of American Association for the Advancement of Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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        Value: 10.1126/science.adx5816
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