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| 42 | + |
| 43 | + |
| 44 | + |
| 45 | +<div id="title"> |
| 46 | + |
| 47 | +# The gas mass reservoir of quiescent galaxies at cosmic noon |
| 48 | + |
| 49 | +</div> |
| 50 | +<div id="comments"> |
| 51 | + |
| 52 | +[](https://arxiv.org/abs/2303.12110)<mark>Appeared on: 2023-03-23</mark> - _Accepted to A&A on the 16/03/2023_ |
| 53 | + |
| 54 | +</div> |
| 55 | +<div id="authors"> |
| 56 | + |
| 57 | +David Blánquez-Sesé, et al. -- incl., <mark>E. Schinnerer</mark> |
| 58 | + |
| 59 | +</div> |
| 60 | +<div id="abstract"> |
| 61 | + |
| 62 | +**Abstract:** We present a 1.1mm stacking analysis of moderately massive (log( $\Mstar$ / $\Msol$ ) = 10.7 $\pm$ 0.2) quiescent galaxies (QGs) at $\langle z\rangle \sim1.5$ , searching for cold dust continuum emission, an excellent tracer of dust and gas mass. Using both the recent GOODS-ALMA survey as well as the full suite of ALMA Band-6 ancillary data in the GOODS-S field, we report the tentative detection of dust continuum equivalent of dust mass log( $\Mdust$ / $\Msol$ ) = 7.47 $\pm$ 0.13 and gas mass log( $\Mgas$ / $\Msol$ ) = 9.42 $\pm$ 0.14. The emerging gas fraction is $\fgas$ = 5.3 $\pm$ 1.8 \% , consistent with the results of previous stacking analyses based on lower resolution sub(mm) observations. Our results support the scenario where high $-z$ QGs have an order of magnitude larger $\fgas$ compared to their local counterparts and have experienced quenching with a non negligible gas reservoir in their interstellar medium - i.e. with gas retention. Subsequent analysis yields an anti-correlation between the $\fgas$ and the stellar mass of QGs, especially in the high mass end where galaxies reside in the most massive haloes. The $\fgas$ - $\Mstar$ anti-correlation promotes the selection bias as a possible solution to the tension between the stacking results pointing towards gas retention in high $-z$ QGs of moderate $\Mstar$ and the studies of individual targets that favour a fully depleted ISM in massive (log( $\Mstar$ / $\Msol$ ) > 11.2) high $-z$ QGs. |
| 63 | + |
| 64 | +</div> |
| 65 | + |
| 66 | +<div id="div_fig1"> |
| 67 | + |
| 68 | +<img src="tmp_2303.12110/./Figures/f_gas_final.png" alt="Fig6.1" width="50%"/><img src="tmp_2303.12110/./Figures/fgas_mstar_15.0.png" alt="Fig6.2" width="50%"/> |
| 69 | + |
| 70 | +**Figure 6. -** **Gas and dust fractions of QGs**_Top_: Selection of $\fdust$ and $\fgas$ measurements as a function of redshift for QGs. Circles correspond to dust derived gas fractions: this work and previous stacks studies ($\Gobat$ and $\Magdis$) are shown in red and blue, respectively. The white circles show two different estimates (connected by a grey dotted line) for a sample of individually observed lensed galaxies. The lower values correspond to those presented in ([Whitaker, Williams and Mowla (2021)]()) and the upper values show the new estimates provided in ([Gobat and Liu (2022)]()) . The grey diamonds represent CO derived $\fgas$ estimates ([Sargent, Daddi and Bournaud 2015](), [Bezanson, Spilker and Williams 2019](), [Williams, Spilker and Whitaker 2021]()) . The red dashed area embeds $\fgas$ measurements of local QGs obtained for the ATLAS3D sample ([Young, Bureau and Davis 2011](), [Cappellari, McDermid and Alatalo 2013](), [Davis, Young and Crocker 2014]()) . The blue shaded area and the purple dashed line represent the best fit to the $\Magdis$ data and the ([Gobat, Magdis and Valentino (2020)]()) model respectively. For reference, we add the $\fgas$ evolution of main sequence galaxies according to ([Liu, Lang and Magnelli (2019)]()) . _Bottom_: Dust and gas fraction as a function of stellar mass for measurements at $z \sim 1.5$. The symbols are the same as in the top panel. The dotted line shows the $\fgas$ prediction according to the ([Davé, Finlator and Oppenheimer (2012)]()) galaxy evolution models, color coded as a function of $M_{\mathrm{halo}}$. For reference, we add the $\fgas$ - $\Mstar$ trend measured by ([Magdis, Daddi and Béthermin (2012)](), [Liu, Lang and Magnelli (2019)]()) . The light yellow scattered diamonds and arrows mark the $\fgas$ detections and upper limits for local QGs with the corresponding best fit plotted as a black dashed line. (*fig:f_gas_plot*) |
| 71 | + |
| 72 | +</div> |
| 73 | +<div id="div_fig2"> |
| 74 | + |
| 75 | +<img src="tmp_2303.12110/./Figures/Galaxy_selection_2.png" alt="Fig1" width="100%"/> |
| 76 | + |
| 77 | +**Figure 1. -** **Galaxy selection.** Density plot of the used ZFOURGE catalogue in the redshift vs stellar mass plane, consisting of a total 13299 galaxies. The red shaded area represents the region covered by our redshift and stellar mass selection criteria ($1 < z < 3$ and 10.20 $<$ log($\Mstar$/$\Msol$) $<$ 11.50) embedding 852 sources. The orange circles correspond to the QGs that constitute our final selection. (*fig:galaxy_selection*) |
| 78 | + |
| 79 | +</div> |
| 80 | +<div id="div_fig3"> |
| 81 | + |
| 82 | +<img src="tmp_2303.12110/./Figures/UVJ_diagram.png" alt="Fig2" width="100%"/> |
| 83 | + |
| 84 | +**Figure 2. -** **UVJ colour diagram.** Distribution of the parent sample of 435 galaxies that meet our selection criteria in the $U-V$, $V-J$ colour-colour space, colour coded by their log(SFR). The red box represents the quiescent region limits defined in ([Schreiber, Pannella and Elbaz (2015)]()) , which enclose the 140 QGs from which we draw our final sample. (*fig:UVJ_diagram*) |
| 85 | + |
| 86 | +</div> |
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