Molecular Emission from a Galaxy Associated with a z ̃ 2.2 Damped Lyα Absorber

Neeleman, Marcel; Kanekar, Nissim; Prochaska, J. Xavier; Christensen, Lise; Dessauges-Zavadsky, Miroslava; Fynbo, Johan P. U.; Møller, Palle; Zwaan, Martin A.

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Molecular Emission from a Galaxy Associated with a z ̃ 2.2 Damped Lyα Absorber

MPS-Authors

Neeleman, Marcel
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kanekar, Nissim
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Prochaska, J. Xavier
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Christensen, Lise
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Dessauges-Zavadsky, Miroslava
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fynbo, Johan P. U.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Møller, Palle
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zwaan, Martin A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018ApJ...856L..12N
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引用

Neeleman, M., Kanekar, N., Prochaska, J. X., Christensen, L., Dessauges-Zavadsky, M., Fynbo, J. P. U., Møller, P., & Zwaan, M. A. (2018). Molecular Emission from a Galaxy Associated with a z ̃ 2.2 Damped Lyα Absorber. The Astrophysical Journal, 856.

引用: https://hdl.handle.net/21.11116/0000-0005-CBFA-D

要旨

Using the Atacama Large Millimeter/submillimeter Array, we have detected CO(3-2) line and far-infrared continuum emission from a galaxy associated with a high-metallicity ([M/H] = -0.27) damped Lyα absorber (DLA) at z _DLA = 2.19289. The galaxy is located 3.″5 away from the quasar sightline, corresponding to a large impact parameter of 30 kpc at the DLA redshift. We use archival Very Large Telescope-SINFONI data to detect Hα emission from the associated galaxy, and find that the object is dusty, with a dust-corrected star formation rate of {110}_-30⁺⁶⁰ M_☉ yr^-1. The galaxy’s molecular mass is large, M_mol = (1.4 ± 0.2) × 10¹¹ × (α _CO/4.3) × (0.57/r ₃₁) M _☉, supporting the hypothesis that high-metallicity DLAs arise predominantly near massive galaxies. The excellent agreement in redshift between the CO(3-2) line emission and low-ion metal absorption (̃40 km s^-1) disfavors scenarios whereby the gas probed by the DLA shows bulk motion around the galaxy. We use Giant Metrewave Radio Telescope H I 21 cm absorption spectroscopy to find that the H I along the DLA sightline must be warm, with a stringent lower limit on the spin temperature of T _s > 1895 × (f/0.93) K. The detection of C I absorption in the DLA, however, also indicates the presence of cold neutral gas. To reconcile these results requires that the cold components in the DLA contribute little to the H I column density, yet contain roughly 50% of the metals of the absorber, underlining the complex multi-phase nature of the gas surrounding high-z galaxies.