Star formation and AGN activity in SDSS cluster galaxies

Linden, Anja von der; Wild, Vivienne; Kauffmann, Guinevere; White, Simon D. M.; Weinmann, Simone M.

doi:10.1111/j.1365-2966.2010.16375.x

Cited by 196 publications

(209 citation statements)

References 97 publications

(140 reference statements)

Supporting

Mentioning

183

Contrasting

Unclassified

Order By: Relevance

“…Our analysis, which adopts the criteria of Cid Fernandes et al (2010Fernandes et al ( , 2011 for the classification of nuclei, is in full agreement with both Kauffmann et al (2004) and Von der Linden et al (2010). We conclude that, even after eliminating the effects of morphology segregation (by counting the frequency of nuclear activity in the proper bins of Hubble type), there is a residual decline in the frequency of nuclear activity (either triggered by black holes or sustained by the star formation) with increasing galaxy density (see Fig.…”

Section: Discussionsupporting

confidence: 77%

“…The decrease in their frequency with increasing galaxy density is mostly due to the decrease in the frequency of galaxies that are able to host AGNs (morphology segregation), but − to a lesser extent -is due to a genuine extra decrease in AGN frequency in high density environments. Von der Linden et al (2010) argued that galaxies in dense environments are less likely to host a powerful optical AGN or a star-forming nuclear region. The frequency of optical AGNs in early-type galaxies declines in high density environments (by approximately a factor of two between the field and the center of clusters).…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

The complete census of optically selected AGNs in the Coma supercluster: the dependence of AGN activity on the local environment

Gavazzi

Savorgnan

Fumagalli

2011

A&A

View full text Add to dashboard Cite

Aims. To investigate the dependence of the occurrence of active galactic nuclei (AGNs) on local galaxy density, we study the nuclear properties of ∼5000 galaxies in the Coma supercluster whose density spans two orders of magnitude from the sparse filaments to the cores of rich clusters. Methods. We obtained optical spectra of the nuclei of 283 galaxies using the 1.5 m Cassini telescope of Bologna observatory. Among these galaxies, 177 belong to the Coma supercluster and are added to the 4785 spectra available from SDSS (DR7) to fill-in the incomplete coverage by SDSS of luminous galaxies. We perform a spectral classification of the nuclei of galaxies in this region (with a completeness of 98% at r ≤ 17.77), classifying the nuclear spectra in six classes: three of them (SEY, sAGN, LIN) refer to AGNs and the remaining three (HII, RET, PAS) refer to different stages of starburst activity. We perform this classification as recommended by Cid Fernandes and collaborators using the ratio of λ 6584 [NII] to Hα lines and the equivalent width of Hα (WHAN diagnostic), after correcting the last quantity by 1.3 Å for underlying absorption. Results. We find that 482 (10%) of 5027 galaxies host an AGN: their frequency strongly increases with increasing luminosity of the parent galaxies, such that 32% of galaxies with Log(L i /L ) ≥ 10.2 harbor an AGN at their interior. In addition to their presence in luminous galaxies, AGNs are also found in red galaxies with g−i 1.15±0.15 mag. The majority of SEY and sAGN (strong AGNs) are associated with luminous late-type (or S0a) galaxies, while LIN (weak AGNs) and RET ("retired": nuclei that have experienced a starburst phase in the past and are now ionized by their hot evolved low-mass stars), are mostly found among E/S0as. The number density of AGNs, HII region-like, and retired galaxies is found to anti-correlate with the local density of galaxies, such that their frequency drops by a factor of two near the cluster cores, while the frequency of galaxies containing passive nuclei increases by the same amount towards the center of rich clusters. The dependence of AGN number density on the local galaxy density is greater than the one implied by morphology segregation alone.

show abstract

Section: Discussionsupporting

confidence: 77%

Section: Discussionmentioning

confidence: 99%

The complete census of optically selected AGNs in the Coma supercluster: the dependence of AGN activity on the local environment

Gavazzi

Savorgnan

Fumagalli

2011

A&A

View full text Add to dashboard Cite

show abstract

“…Some observational studies (e.g. Balogh et al 2000;Haines et al 2009;von der Linden et al 2010;Rasmussen et al 2012;Geha et al 2012) find an enhanced quiescent fraction of centrals in the vicinity of massive neighbour haloes out to four times the virial radius. Other studies find, however, no such trend.…”

Section: Introductionmentioning

confidence: 99%

The influence of the environmental history on quenching star formation in a Λ cold dark matter universe

Hirschmann¹,

Lucia²,

Wilman³

et al. 2014

Monthly Notices of the Royal Astronomical Society

Self Cite

113

145

View full text Add to dashboard Cite

We present a detailed analysis of the influence of the environment and of the environmental history on quenching star formation in central and satellite galaxies in the local Universe. We take advantage of publicly available galaxy catalogues obtained from applying a galaxy formation model to the Millennium simulation. In addition to halo mass, we consider the local density of galaxies within various fixed scales. Comparing our model predictions to observational data (SDSS), we demonstrate that the models are failing to reproduce the observed density dependence of the quiescent galaxy fraction in several aspects: for most of the stellar mass ranges and densities explored, models cannot reproduce the observed similar behaviour of centrals and satellites, they slightly under-estimate the quiescent fraction of centrals and significantly overestimate that of satellites. We show that in the models, the density dependence of the quiescent central galaxies is caused by a fraction of "backsplash" centrals which have been satellites in the past. The observed stronger density dependence on scales of 0.2 − 1 Mpc may, however, indicate additional environmental processes working on central galaxies. Turning to satellite galaxies, the density dependence of their quiescent fractions reflects a dependence on the time spent orbiting within a parent halo, correlating strongly with halo mass and distance from the halo centre. Comparisons with observational estimates suggest relatively long gas consumption time scales of roughly 5 Gyr in low mass satellite galaxies. The quenching time scales decrease with increasing satellite stellar mass. Overall, a change in modelling both internal processes and environmental processes is required for improving currently used galaxy formation models.

show abstract

“…A spectroscopic study of 521 clusters in the SDSS by von der Linden et al (2010) indicated that the star formation rates of galaxies decline slowly during the infall into a cluster, with the most rapid quenching only occurring at the centres of clusters. The inferred quenching timescales were therefore long, roughly a few Gyrs, which is comparable to the cluster crossing time.…”

Section: Introductionmentioning

confidence: 99%

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Schaefer

Croom

Allen

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph (SAMI) Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially-resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M * ; 10 8.1 -10 10.95 M ) and in 5 th nearest neighbour local environment density (Σ 5 ; 10 −1.3 -10 2.1 Mpc −2 ). We show that star formation rate gradients in galaxies are steeper in dense (log 10 (Σ 5 /Mpc 2 ) > 0.5) environments by 0.58 ± 0.29 dex r e −1 in galaxies with stellar masses in the range 10 10 < M * /M < 10 11 and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density the star-formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scaleradius ratio (r 50,Hα /r 50,cont ), which compares the extent of ongoing star formation to previous star formation. With this metric we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ∼ 5 ± 4% in low-density environments (log 10 (Σ 5 /Mpc 2 ) < 0.0) to 30 ± 15% in the highest density environments (log 10 (Σ 5 /Mpc 2 ) > 1.0). These lines of evidence strongly suggest that with increasing local environment density the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.

show abstract

Star formation and AGN activity in SDSS cluster galaxies

Cited by 196 publications

References 97 publications

The complete census of optically selected AGNs in the Coma supercluster: the dependence of AGN activity on the local environment

The complete census of optically selected AGNs in the Coma supercluster: the dependence of AGN activity on the local environment

The influence of the environmental history on quenching star formation in a Λ cold dark matter universe

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Contact Info

Product

Resources

About