The Large Early Galaxy Astrophysics Census (LEGA-C) Data Release 3: 3000 High-quality Spectra of K
               <sub>
                  s
               </sub>-selected Galaxies at z &gt; 0.6

Wel, Arjen van der; Bezanson, Rachel; D’Eugenio, Francesco; Straatman, Caroline; Franx, Marijn; Houdt, Josha van; Maseda, Michael V.; Gallazzi, Anna; Wu, Po-Feng; Pacifici, Camilla; Barišić, Ivana; Brammer, Gabriel; Muñoz-Mateos, J. C.; Vervalcke, Sarah; Zibetti, S.; Sobral, David; Graaff, Anna de; Calhau, João; Kaushal, Yasha; Muzzin, Adam; Bell, Eric F.; Dokkum, Pieter van

doi:10.3847/1538-4365/ac1356

Cited by 62 publications

(10 citation statements)

References 69 publications

(77 reference statements)

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“…We exclude sources with FLAG_SPEC = 2, that indicates that the photometry based flux calibration showed significant imperfections, compromising the measurement of absorption and emission indices (sect. 4.2 in van der Wel et al 2021). We further exclude sources with FLAG_MORPH = 1 or 2.…”

Section: Final Lega-c Samplesmentioning

confidence: 99%

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Comparison of star formation histories of AGN and non-AGN galaxies

Mountrichas

Buat

Yang

et al. 2022

A&A

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We use AGN with X-ray luminosities, L X,2−10keV ∼ 10 42.5−44 erg s −1 , from the COSMOS-Legacy survey that lie within the UltraVISTA region and cross match them with the LEGA-C catalogue. The latter provides measurements of the calcium break, D n 4000, and H δ Balmer line that allow us to study the stellar populations of AGN and compare them with a galaxy reference catalogue. Our samples consist of 69 AGN and 2176 non-AGN systems, within 0.6 < z < 1.3, that satisfy the same photometric selection criteria. We construct the SEDs of both population and use the CIGALE code to investigate the effect of the two indices in the SED fitting process. Our analysis shows that the inclusion of D n 4000 and H δ allows CIGALE to constrain better the ages of the stellar populations. Furthermore, we find an increase of the estimated stellar masses by, on average, ∼ 0.2 dex, in particular for systems with young stars (D n 4000 < 1.5), when the two indices are included in the SED fitting. We then compare the D n 4000 and H δ of AGN with sources in the reference catalogue, accounting for the different stellar mass of the two populations. Our analysis reveals that low to moderate L X AGN tend to reside in galaxies with older stellar populations and are less likely to have experienced a recent star formation burst, compared to galaxies in the control sample. Finally, we compare the two populations as a function of their morphology (bulgedominated, BD, vs. non-BD) and compactness (mass-to-size ratio). A similar fraction of AGN and non-AGN systems are classified as non-BD (∼ 70%). Our analysis shows that BD AGN tend to have younger stellar populations compared to BD, non-AGN systems. On the other hand, non-BD AGN have, on average, older stellar populations and are less likely to have experienced a burst compared to non-BD sources in the reference sample. Furthermore, AGN tend to prefer more compact systems compared to non-AGN.

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Section: Final Lega-c Samplesmentioning

confidence: 99%

“…Finally, we use line indices only for galaxies that have a measured stellar velocity dispersion (sect. 3.4 in van der Wel et al 2021). These criteria reduce the number of X-ray AGN to 94 and the number of galaxies to 2834, within 0.6 < z < 1.3.…”

Section: Final Lega-c Samplesmentioning

confidence: 99%

Comparison of star formation histories of AGN and non-AGN galaxies

Mountrichas

Buat

Yang

et al. 2022

A&A

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“…4.2). For that purpose, we cross-match our AGN and galaxies in the control sample with the LEGA-C catalogue (van der Wel et al 2016;Straatman et al 2018;van der Wel et al 2021). This catalogue includes spectra for 4081 galaxies (3741 unique objecs) within 0.6 < z < 1.3.…”

Section: Star-formation Historymentioning

confidence: 99%

The relation of cosmic environment and morphology with the star formation and stellar populations of AGN and non-AGN galaxies

Mountrichas

Yang

Buat

et al. 2023

A&A

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In this work, we study the relation of the cosmic environment and morphology with the star formation and stellar population of galaxies. Most importantly, we examine if this relation differs for systems with active and non-active supermassive black holes. For that purpose, we used 551 X-ray detected active galactic nuclei (AGNs) and 16 917 non-AGN galaxies in the COSMOS-Legacy survey for which surface-density field measurements are available. The sources lie at a redshift of 0.3 < z < 1.2, probe X-ray luminosities of 42 < log[LX,2−10 keV(erg s−1)] < 44, and have stellar masses of 10.5 < log [M*(M⊙)] < 11.5. Our results show that isolated AGNs (field) have lower star formation rates (SFRs) compared to non-AGNs at all LX spanned by our sample. However, in denser environments (filaments and clusters), moderate LX AGN (log[LX,2−10 keV(erg s−1)] > 43) and non-AGN galaxies have similar SFRs. We also examined the stellar populations and the morphology of the sources in different cosmic fields. For the same morphological type, we find that non-AGN galaxies tend to have older stellar populations and are less likely to have undergone a recent burst in denser environments compared to their field counterparts. The differences in the stellar populations concerning density field are mainly driven by quiescent systems. Moreover, low LX AGNs present negligible variations of their stellar populations in all cosmic environments, whereas moderate LX AGNs have, on average, younger stellar populations and are more likely to have undergone a recent burst in high-density fields. Finally, in the case of non-AGN galaxies, the fraction of bulge-dominated (BD) systems increases with the density field, while BD AGNs are scarce in denser environments. Our results are consistent with a scenario in which a common mechanism, such as mergers, triggers both the star-formation and the AGN activity.

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“…In Figure 15 we plot our sample as a combined median where σ is the median of all the line moment measurements presented in Section 3.2, which is 260±21 km s −1 . As a comparison measurements of local ETGs that are based on the MASSIVE (Davis et al 2019) and ATLAS 3D (Cappellari et al 2013) surveys are shown, as well as the quiescent galaxies (D n 4000> 1.55; Kauffmann et al 2003;Wu et al 2018) at z = 0.6 − 1.0 based on the LEGA-C survey (van der Wel et al 2021;Wu et al 2021) and some compiled z ∼ 2 − 4 spectroscopically confirmed quiescent galaxies (Stockmann et al 2020;Valentino et al 2020). The results from the simi-8 re = 1.68h for an exponential disk profile (Chen et al 2015) lar analyses of mostly fainter SMGs presented by Birkin et al (2021) are also shown.…”

Section: Connecting To the Descendantsmentioning

confidence: 99%

An ALMA Spectroscopic Survey of the Brightest Submillimeter Galaxies in the SCUBA-2-COSMOS field (AS2COSPEC): Survey Description and First Results

Chen,

Liao,

Smail

et al. 2021

Preprint

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We introduce an ALMA band 3 spectroscopic survey, targeting the brightest submillimeter galaxies (SMGs) in the COSMOS field. Here we present the first results based on the 18 primary SMGs that have 870 µm flux densities of S 870 = 12.4 − 19.3 mJy and are drawn from a parent sample of 260 ALMA-detected SMGs from the AS2COSMOS survey. We detect emission lines in 17 and determine their redshifts to be in the range of z = 2 − 5 with a median of 3.2 ± 0.3. We confirm that SMGs with brighter S 870 are located at higher redshifts. The data additionally cover five fainter companion SMGs, and we obtain line detection in one. Together with previous studies, our results indicate that for SMGs that satisfy our selection, their brightest companion SMGs are physically associated with their corresponding primary SMGs in ≥ 40% of the time, suggesting that mergers play a role in the triggering of star formation. By modeling the foreground gravitational fields, < 10% of the primary SMGs can be strongly lensed with a magnification µ > 2. We determine that about 90% of the primary SMGs have lines that are better described by double Gaussian profiles, and the median separation of the two Gaussian peaks is 430±40 km s −1 . This allows estimates of an average baryon mass, which together with the line dispersion measurements puts our primary SMGs on the similar mass-σ correlation found on local early-type galaxies. Finally, the number density of our z > 4 primary SMGs is found to be 1 × 10 −6 cMpc −3 , suggesting that they can be the progenitors of z ∼ 3 − 4 massive quiescent galaxies.

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The Large Early Galaxy Astrophysics Census (LEGA-C) Data Release 3: 3000 High-quality Spectra of K _s-selected Galaxies at z > 0.6

Cited by 62 publications

References 69 publications

Comparison of star formation histories of AGN and non-AGN galaxies

Comparison of star formation histories of AGN and non-AGN galaxies

The relation of cosmic environment and morphology with the star formation and stellar populations of AGN and non-AGN galaxies

An ALMA Spectroscopic Survey of the Brightest Submillimeter Galaxies in the SCUBA-2-COSMOS field (AS2COSPEC): Survey Description and First Results

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The Large Early Galaxy Astrophysics Census (LEGA-C) Data Release 3: 3000 High-quality Spectra of K s -selected Galaxies at z > 0.6

Cited by 62 publications

References 69 publications

Comparison of star formation histories of AGN and non-AGN galaxies

Comparison of star formation histories of AGN and non-AGN galaxies

The relation of cosmic environment and morphology with the star formation and stellar populations of AGN and non-AGN galaxies

An ALMA Spectroscopic Survey of the Brightest Submillimeter Galaxies in the SCUBA-2-COSMOS field (AS2COSPEC): Survey Description and First Results

Contact Info

Product

Resources

About

The Large Early Galaxy Astrophysics Census (LEGA-C) Data Release 3: 3000 High-quality Spectra of K _s-selected Galaxies at z > 0.6