Galaxy kinematics and mass estimates at $z\sim1$ from ionised gas and stars
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2022
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866910572332711936 |
|---|---|
| author | Übler, Hannah Schreiber, Natascha M. Förster van der Wel, Arjen Bezanson, Rachel Price, Sedona H. D'Eugenio, Francesco Wisnioski, Emily Genzel, Reinhard Tacconi, Linda J. Wuyts, Stijn Naab, Thorsten Lutz, Dieter Straatman, Caroline M. S. Shimizu, T. Taro Davies, Ric Liu, Daizhong Mendel, J. Trevor |
| author_facet | Übler, Hannah Schreiber, Natascha M. Förster van der Wel, Arjen Bezanson, Rachel Price, Sedona H. D'Eugenio, Francesco Wisnioski, Emily Genzel, Reinhard Tacconi, Linda J. Wuyts, Stijn Naab, Thorsten Lutz, Dieter Straatman, Caroline M. S. Shimizu, T. Taro Davies, Ric Liu, Daizhong Mendel, J. Trevor |
| contents | We compare ionised gas and stellar kinematics of 16 star-forming galaxies ($\log(M_\star/M_\odot)=9.7-11.2$, SFR=6-86 $M_\odot/yr$) at $z\sim1$ using near-infrared integral field spectroscopy (IFS) of H$α$ emission from the KMOS$^{\rm 3D}$ survey and optical slit spectroscopy of stellar absorption and gas emission from the LEGA-C survey. H$α$ is dynamically colder than stars, with higher disc rotation velocities (by ~45 per cent) and lower disc velocity dispersions (by a factor ~2). This is similar to trends observed in the local Universe. We find higher rotational support for H$α$ relative to [OII], potentially explaining systematic offsets in kinematic scaling relations found in the literature. Regarding dynamical mass measurements, for six galaxies with cumulative mass profiles from Jeans Anisotropic Multi-Gaussian Expansion (JAM) models the H$α$ dynamical mass models agree remarkably well out to ~10 kpc for all but one galaxy (average $ΔM_{\rm dyn}(R_{e,\rm F814W})<0.1$ dex). Simpler dynamical mass estimates based on integrated stellar velocity dispersion are less accurate (standard deviation 0.24 dex). Differences in dynamical mass estimates are larger, for example, for galaxies with stronger misalignments of the H$α$ kinematic major axis and the photometric position angle, highlighting the added value of IFS observations for dynamics studies. The good agreement between the JAM models and the dynamical models based on H$α$ kinematics at $z\sim1$ corroborates the validity of dynamical mass measurements from H$α$ IFS observations also for higher redshift rotating disc galaxies. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2210_03106 |
| institution | arXiv |
| publishDate | 2022 |
| record_format | arxiv |
| spellingShingle | Galaxy kinematics and mass estimates at $z\sim1$ from ionised gas and stars Übler, Hannah Schreiber, Natascha M. Förster van der Wel, Arjen Bezanson, Rachel Price, Sedona H. D'Eugenio, Francesco Wisnioski, Emily Genzel, Reinhard Tacconi, Linda J. Wuyts, Stijn Naab, Thorsten Lutz, Dieter Straatman, Caroline M. S. Shimizu, T. Taro Davies, Ric Liu, Daizhong Mendel, J. Trevor Astrophysics of Galaxies We compare ionised gas and stellar kinematics of 16 star-forming galaxies ($\log(M_\star/M_\odot)=9.7-11.2$, SFR=6-86 $M_\odot/yr$) at $z\sim1$ using near-infrared integral field spectroscopy (IFS) of H$α$ emission from the KMOS$^{\rm 3D}$ survey and optical slit spectroscopy of stellar absorption and gas emission from the LEGA-C survey. H$α$ is dynamically colder than stars, with higher disc rotation velocities (by ~45 per cent) and lower disc velocity dispersions (by a factor ~2). This is similar to trends observed in the local Universe. We find higher rotational support for H$α$ relative to [OII], potentially explaining systematic offsets in kinematic scaling relations found in the literature. Regarding dynamical mass measurements, for six galaxies with cumulative mass profiles from Jeans Anisotropic Multi-Gaussian Expansion (JAM) models the H$α$ dynamical mass models agree remarkably well out to ~10 kpc for all but one galaxy (average $ΔM_{\rm dyn}(R_{e,\rm F814W})<0.1$ dex). Simpler dynamical mass estimates based on integrated stellar velocity dispersion are less accurate (standard deviation 0.24 dex). Differences in dynamical mass estimates are larger, for example, for galaxies with stronger misalignments of the H$α$ kinematic major axis and the photometric position angle, highlighting the added value of IFS observations for dynamics studies. The good agreement between the JAM models and the dynamical models based on H$α$ kinematics at $z\sim1$ corroborates the validity of dynamical mass measurements from H$α$ IFS observations also for higher redshift rotating disc galaxies. |
| title | Galaxy kinematics and mass estimates at $z\sim1$ from ionised gas and stars |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2210.03106 |