The rise and fall of star formation in z ∼ 0.2 merging galaxy clusters

Stroe, Andra; Sobral, David; Dawson, William A.; Jee, M. James; Hoekstra, Henk; Wittman, David; Weeren, R. J. van; Brüggen, M.; Röttgering, H. J. A.

doi:10.1093/mnras/stu2519

Cited by 70 publications

(99 citation statements)

References 96 publications

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“…The density is about ∼ 16 emitters per square degree, densities similar to the densest parts of our wide, shallow Hα survey. Our results thus corroborate the conclusions from Stroe et al (2014) and Stroe et al (2015).…”

Section: Distribution Of Hα Emitterssupporting

confidence: 91%

“…Spectroscopic observations using NB1 and NB2 (e.g Stroe et al 2015;Sobral et al 2015a) confirm the presence of such stars. All the sources masked as stars are removed from catalogues such that they are not selected as line emitters.…”

Section: Star Removalmentioning

confidence: 78%

“…We obtained narrow band data using the NOVA782HA and NOVA804HA (Stroe et al 2014(Stroe et al , 2015Sobral et al 2015a) filters on the Wide Wide Field Camera (WFC) 1 mounted on the Isaac Newton Telescope (INT, I13BN008, PI Sobral) 2 . For brevity, we label the filters as NB1 (NOVA782HA) and NB2 (NOVA804HA).…”

Section: Narrow Band Hα Observationsmentioning

confidence: 99%

“…However, given the WFC focal ratio ( f /3.29), this effect is expected to be very low (a few per cent Bland-Hawthorn et al 2001). Sobral et al (2015a) and Stroe et al (2015) characterised the filters with spectroscopy from the Keck and Willam Herschel Telescopes with sources located both towards Figure 1. Colour-colour plots for the SA22, W2 and XMMLSS fields, mainly used to remove stars.…”

Section: Narrow Band Hα Observationsmentioning

confidence: 99%

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A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

Stroe

Sobral

2015

Mon. Not. R. Astron. Soc.

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We carried out the largest (> 3.5 × 10 5 Mpc 3 , 26 deg 2 ) Hα narrow band survey to date at z ∼ 0.2 in the SA22, W2 and XMMLSS extragalactic fields. Our survey covers a large enough volume to overcome cosmic variance and to sample bright and rare Hα emitters up to an observed luminosity of ∼ 10 42.4 erg s −1 , equivalent to ∼ 11M yr −1 . Using our sample of 220 sources brighter than > 10 41.4 erg s −1 (> 1M yr −1 ), we derive Hα luminosity functions, which are well described by a Schechter function with φ * = 10 −2.85±0.03 Mpc −3 and L * Hα = 10 41.71±0.02 erg s −1 (with a fixed faint end slope α = −1.35). We find that surveys probing smaller volumes (∼ 3 × 10 4 Mpc 3 ) are heavily affected by cosmic variance, which can lead to errors of over 100 per cent in the characteristic density and luminosity of the Hα luminosity function. We derive a star formation rate density of ρ SFRD = 0.0094 ± 0.0008 M yr −1 , in agreement with the redshift-dependent Hα parametrisation from Sobral et al. (2013). The two-point correlation function is described by a single power law ω(θ ) = (0.159 ± 0.012)θ (−0.75±0.05) , corresponding to a clustering length of r 0 = 3.3 ± 0.8 Mpc/h. We find that the most luminous Hα emitters at z ∼ 0.2 are more strongly clustered than the relatively fainter ones. The L * Hα Hα emitters at z ∼ 0.2 in our sample reside in ∼ 10 12.5−13.5 M dark matter haloes. This implies that the most star forming galaxies always reside in relatively massive haloes or group-like environments and that the typical host halo mass of star-forming galaxies is independent of redshift if scaled by L Hα /L * Hα (z), as proposed by Sobral et al. (2010).

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Section: Distribution Of Hα Emitterssupporting

confidence: 91%

Section: Star Removalmentioning

confidence: 78%

Section: Narrow Band Hα Observationsmentioning

confidence: 99%

Section: Narrow Band Hα Observationsmentioning

confidence: 99%

See 2 more Smart Citations

A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

Stroe

Sobral

2015

Mon. Not. R. Astron. Soc.

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“…The high ρ * , and hence high ρ SFR , defines the visible baryonic component of the protocluster. This is the same situation as in the nearby Universe, where the ρ SFR within clusters is typically two orders of magnitude greater than the field (Stroe et al 2015;Guglielmo et al 2015) due to the high galaxy density.…”

Section: Dense Environments Suppress Star Formationmentioning

confidence: 53%

The impact of protocluster environments atz= 1.6

Hatch

Cooke

Muldrew

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigate the effects of dense environments on galaxy evolution by examining how the properties of galaxies in the z = 1.6 protocluster Cl 0218.3−0510 depend on their location. We determine galaxy properties using spectral energy distribution fitting to 14-band photometry, including data at three wavelengths that tightly bracket the Balmer and 4000Å breaks of the protocluster galaxies. We find that two-thirds of the protocluster galaxies, which lie between several compact groups, are indistinguishable from field galaxies. The other third, which reside within the groups, differ significantly from the intergroup galaxies in both colour and specific star formation rate. We find that the fraction of red galaxies within the massive protocluster groups is twice that of the intergroup region. These excess red galaxies are due to enhanced fractions of both passive galaxies (1.7 times that of the intergroup region) and dusty star-forming galaxies (3 times that of the intergroup region). We infer that some protocluster galaxies are processed in the groups before the cluster collapses. These processes act to suppress star formation and change the mode of star formation from unobscured to obscured.

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