The Environment of Passive Spiral Galaxies in the SDSS

Goto, Tomotsugu; Okamura, S.; Sekiguchi, M.; Bernardi, Mariangela; Brinkmann, J.; Gómez, Percy; Harvanek, Michael; Kleinman, S. J.; Krzesiński, Jurek; Long, D.; Loveday, Jon; Miller, Christopher J.; Neilsen, Eric H.; Newman, Peter R.; Nitta, A.; Sheth, Ravi K.; Snedden, Stephanie A.; Yamauchi, Chisato

doi:10.1093/pasj/55.4.757

Cited by 125 publications

(122 citation statements)

References 99 publications

(131 reference statements)

Supporting

Mentioning

112

Contrasting

Order By: Relevance

“…However, many field E+A galaxies indicate that explaining cluster galaxy evolution through E+A galaxies is perhaps not plausible any more. Passive spiral galaxies (Goto et al 2003e;Yamauchi & Goto 2004) may be an alternative candidate for the transition objects in cluster regions instead of E+As.…”

Section: Discussionmentioning

confidence: 99%

Are E+A galaxies dusty-starbursts?: VLA 20 cm radio continuum observation

Goto¹

2004

A&A

View full text Add to dashboard Cite

Abstract. E+A galaxies are characterized as a galaxy with strong Balmer absorption lines but without any [OII] or Hα emission lines. The existence of strong Balmer absorption lines means that E+A galaxies have experienced a starburst within the last <1-1.5 Gyr. However, the lack of [OII] or Hα emission lines indicates that E+A galaxies do not have any on-going star formation. Therefore, E+A galaxies are interpreted as a post-starburst galaxy. For more than 20 years, however, it has been a mystery why E+A galaxies underwent a starburst then stopped abruptly. One possible explanation to E+A galaxies is the dusty starburst scenario, where E+A galaxies have on-going star formation, but optical emission lines are invisible due to the heavy obscuration by dust. To test this dusty starburst scenario, we have observed 36 E+A galaxies carefully selected from the Sloan Digital Sky Survey Data Release 1 in 20 cm radio continuum using the VLA. Since the radio emission is not affected by the dust extinction, the star formation rate (SFR) in dusty galaxies can be revealed by the 20 cm continuum. All of our 36 target E+A galaxies are selected to have Hδ equivalent width greater than 6 Å and no detection of [OII] or Hα emission lines within 1σ. These selection criteria are much stronger than previous E+A selections in our attempt to select galaxies in the pure post-starburst phase without any remaining star formation. Except for the two galaxies with a nearby radio source, none of our 34 E+A galaxies are detected in 20 cm continuum to the limits reported in Table 1. The obtained upper limits on the radio estimated SFR suggest that E+A galaxies do not possess strong starburst (>100 M yr −1 ) hidden by dust extinction for the whole sample while 15 (z < 0.08) E+As have lower SFR upper limits of ∼15 M yr −1 .

show abstract

Section: Discussionmentioning

confidence: 99%

Are E+A galaxies dusty-starbursts?: VLA 20 cm radio continuum observation

Goto¹

2004

A&A

View full text Add to dashboard Cite

show abstract

“…spiral morphology but no star formation), which are considered objects in a transition phase to an early type morphology, tend to be found in this kind of intermediate density regions (e.g. Goto et al 2003). The situation seems to change towards higher redshift.…”

Section: Introductionmentioning

confidence: 91%

The effect of environment on star forming galaxies at redshift

Popesso

Rodighiero

Saintonge

et al. 2011

A&A

View full text Add to dashboard Cite

We use deep 70, 100 and 160 μm observations taken with PACS, the Photodetector Array Camera and Spectrometer on board of Herschel, as part of the PACS Evolutionary Probe (PEP) guaranteed time, to study the relation between star formation rate and environment at redshift ∼1 in the GOODS-S and GOODS-N fields. We use the SDSS spectroscopic catalog to build the local analog and study the evolution of the star formation activity dependence on the environment. At z ∼ 1 we observe a reversal of the relation between star formation rate and local density, confirming the results based on Spitzer 24 μm data. However, due to the high accuracy provided by PACS in measuring the star formation rate also for AGN hosts, we identify in this class of objects the cause for the reversal of the density-SFR relation. Indeed, AGN hosts favor high stellar masses, dense regions and high star formation rates. Without the AGN contribution the relation flattens consistently with respect to the local analog in the same range of star formation rates. As in the local universe, the specific star formation rate anti-correlates with the density. This is due to mass segregation both at high and low redshift. The contribution of AGN hosts does not affect this anti-correlation, since AGN hosts exhibit the same specific star formation rate as star forming galaxies at the same mass. The same global trends and AGN contribution is observed once the relations are studied per morphological type. We study the specific star formation rate vs. stellar mass relation in three density regimes. Our data provides an indication that at M/M > 10 11 the mean specific star formation rate tends to be higher at higher density, while the opposite trend is observed in the local SDSS star forming sample.

show abstract

“…This relation is redshift dependent and while the fraction of elliptical galaxies (∼15%, Vogt et al 2004) does not change with Appendices are only available in electronic form at http://www.aanda.org redshift, the S0 fraction increases with decreasing redshift and the spiral fraction, on the contrary, decreases (Couch et al 1998). The fraction of spirals with no current star formation activity is significantly larger in clusters than in the field (van den Bergh 1976; Poggianti et al 1999;Couch et al 2001;Goto et al 2003;Verdugo et al 2008;Sikkema 2009). Also, distant clusters have a larger fraction of star forming galaxies compared to nearby clusters (Butcher & Oemler 1978, 1984Ellingson et al 2001;Kodama & Bower 2001).…”

Section: Introductionmentioning

confidence: 99%

Internal kinematics of spiral galaxies in distant clusters

Kutdemir

Ziegler

Peletier³

et al. 2010

A&A

View full text Add to dashboard Cite

Aims. We trace the interaction processes of galaxies at intermediate redshift by measuring the irregularity of their ionized gas kinematics, and investigate these irregularities as a function of the environment (cluster versus field) and of morphological type (spiral versus irregular). Methods. We obtain the gas velocity fields by placing three parallel and adjacent VLT/FORS2 slits on each galaxy. To quantify irregularities in the gas kinematics, we use three indicators: the standard deviation of the kinematic position angle (σ PA ), the mean deviation of the line of sight velocity profile from the cosine form which is measured using high order Fourier terms (k 3,5 /k 1 ) and the average misalignment between the kinematical and photometric major axes (Δφ). These indicators are then examined together with some photometric and structural parameters (measured from HST and FORS2 images in the optical) such as the disk scale length, rest-frame colors, asymmetry, concentration, Gini coefficient and M 20 . Our sample consists of 92 distant galaxies. 16 cluster (z ∼ 0.3 and z ∼ 0.5) and 29 field galaxies (0.10 ≤ z ≤ 0.91, mean z = 0.44) of these have velocity fields with sufficient signal to be analyzed. To compare our sample with the local universe, we also analyze a sample from the SINGS survey. Results. We find that the fraction of galaxies that have irregular gas kinematics is remarkably similar in galaxy clusters and in the field at intermediate redshifts (according to σ PA ≈ 10%, k 3,5 /k 1 ≈ 30%, Δφ ≈ 70%). The distribution of the field and cluster galaxies in (ir)regularity parameters space is also similar. On the other hand galaxies with small central concentration of light, that we see in the field sample, are absent in the cluster sample. We find that field galaxies at intermediate redshifts have more irregular velocity fields as well as more clumpy and less centrally concentrated light distributions than their local counterparts. Comparison with a SINS sample of 11 z ∼ 2 galaxies shows that these distant galaxies have more irregular gas kinematics than our intermediate redshift cluster and field sample. We do not find a dependence of the irregularities in gas kinematics on morphological type. We find that two different indicators of star formation correlate with irregularity in the gas kinematics. Conclusions. More irregular gas kinematics, also more clumpy and less centrally concentrated light distributions of spiral field galaxies at intermediate redshifts in comparison to their local counterparts indicate that these galaxies are probably still in the process of building their disks via mechanisms such as accretion and mergers. On the other hand, they have less irregular gas kinematics compared to galaxies at z ∼ 2.

show abstract

The Environment of Passive Spiral Galaxies in the SDSS

Cited by 125 publications

References 99 publications

Are E+A galaxies dusty-starbursts?: VLA 20 cm radio continuum observation

Are E+A galaxies dusty-starbursts?: VLA 20 cm radio continuum observation

The effect of environment on star forming galaxies at redshift

Internal kinematics of spiral galaxies in distant clusters

Contact Info

Product

Resources

About