Stellar Masses From the Candels Survey: The Goods-South and Uds Fields

Santini, P.; Ferguson, Henry C.; Fontana, A.; Mobasher, Bahram; Barro, Guillermo; Castellano, M.; Finkelstein, Steven L.; Grazian, A.; Hsu, Li-Ting; Lee, B.; Lee, Seong-Kook; Pforr, Janine; Salvato, M.; Wiklind, T.; Wuyts, Stijn; Almaini, O.; Cooper, Michael C.; Galametz, A.; Weiner, Benjamin J.; Amorín, R.; Boutsia, K.; Conselice, Christopher J.; Dahlén, T.; Dickinson, Mark; Giavalisco, Mauro; Grogin, Norman A.; Guo, Y.; Hathi, N. P.; Kocevski, Dale D.; Koekemoer, Anton M.; Kurczynski, Peter; Merlin, E.; Mortlock, Alice; Newman, Jeffrey A.; Paris, D.; Pentericci, L.; Simons, Raymond C.; Willner, S. P.

doi:10.1088/0004-637x/801/2/97

Cited by 268 publications

(394 citation statements)

References 85 publications

Supporting

Mentioning

369

Contrasting

Order By: Relevance

“…The offset is defined as log (M CANDELS median /M 3D−HST ). Our offset perfectly matches the median = −0.058 ± 0.003 measured in Santini et al (2015). The authors of the CANDELS stellar mass catalogue argue that, because the comparison is satisfying at a first order, the differences between the two catalogues are due to different systematics in the SED fitting.…”

Section: Stellar Massessupporting

confidence: 80%

“…This diagram is used in many studies to discriminate between SFGs and quiescent galaxies (Williams et al 2009;Patel et al 2012). We took the rest-frame absolute magnitudes from the CANDELS stellar masses catalogue (Santini et al 2015). The catalogue does not provide uncertainties, so we assumed a 0.2 mag photometric uncertainty in the absolute magnitudes, although in SED-fitting derived magnitudes of this kind, the main source for errors is the model assumption.…”

Section: Hα Emitters and Interlopers At Other Redshiftsmentioning

confidence: 99%

“…We were able to see the similarities and differences in terms of blue luminosities (M B ), compactness (effective radius, r e ), and roundness (axis ratio, b/a) with morphology. In this case, we assumed a 0.2 mag photometric uncertainty in the absolute magnitude with the values taken from Santini et al (2015) shown in Fig. 4.…”

Section: Morphologiesmentioning

confidence: 99%

See 2 more Smart Citations

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Gómez-Guijarro

Gallego

Villar

et al. 2016

A&A

View full text Add to dashboard Cite

Context. Studies measuring the star formation rate density, luminosity function, and properties of star-forming galaxies are numerous. However, it exists a gap at 0.5 < z < 0.8 in Hα-based studies. Aims. Our main goal is to study the properties of a sample of faint Hα emitters at z ∼ 0.62. We focus on their contribution to the faint end of the luminosity function and derived star formation rate density, characterising their morphologies and basic photometric and spectroscopic properties. Methods. We use a narrow-band technique in the near-infrared, with a filter centred at 1.06 µm. The data come from ultra-deep VLT/HAWK-I observations in the GOODS-S field with a total of 31.9 h in the narrow-band filter. In addition to our survey, we mainly make use of ancillary data coming from the CANDELS and Rainbow Cosmological Surveys Database, from the 3D-HST for comparison, and also spectra from the literature. We perform a visual classification of the sample and study their morphologies from structural parameters available in CANDELS. In order to obtain the luminosity function, we apply a traditional V/V max method and perform individual extinction corrections for each object to accurately trace the shape of the function. Results. Our 28 Hα-selected sample of faint star-forming galaxies reveals a robust faint-end slope of the luminosity function α = −1.46 +0.16 −0.08 . The derived star formation rate density at z ∼ 0.62 is ρ SFR = 0.036 +0.012 −0.008 M yr −1 Mpc −3 . The sample is mainly composed of disks, but an important contribution of compact galaxies with Sérsic indexes n ∼ 2 display the highest specific star formation rates. Conclusions. The luminosity function at z ∼ 0.62 from our ultra-deep data points towards a steeper α when an individual extinction correction for each object is applied. Compact galaxies are low-mass, low-luminosity, and starburst-dominated objects with a light profile in an intermediate stage from early to late types.

show abstract

Section: Stellar Massessupporting

confidence: 80%

Section: Hα Emitters and Interlopers At Other Redshiftsmentioning

confidence: 99%

See 1 more Smart Citation

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Gómez-Guijarro

Gallego

Villar

et al. 2016

A&A

View full text Add to dashboard Cite

show abstract

“…In particular, photometric redshifts were collected from Luo et al (2010), Rafferty et al (2011), Hsu et al (2014, hereafter H14), Skelton et al (2014, hereafter S14), Santini et al (2015), and Straatman et al (2016, hereafter S16). Each X-ray source can therefore be associated with up to six different photometric redshifts.…”

Section: Agn Parent Sample and Redshifts In The 7 Ms Cdf-smentioning

confidence: 99%

High-redshift AGN in the Chandra Deep Fields: the obscured fraction and space density of the sub-L* population

Vito

Brandt

Yang

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

151

181

View full text Add to dashboard Cite

We investigate the population of high-redshift (3 z < 6) AGN selected in the two deepest X-ray surveys, the 7 Ms Chandra Deep Field-South and 2 Ms Chandra Deep Field-North. Their outstanding sensitivity and spectral characterization of faint sources allow us to focus on the sub-L * regime (logL X 44), poorly sampled by previous works using shallower data, and the obscured population. Taking fully into account the individual photometric-redshift probability distribution functions, the final sample consists of ≈ 102 X-ray selected AGN at 3 z < 6. The fraction of AGN obscured by column densities logN H > 23 is ∼ 0.6 − 0.8, once incompleteness effects are taken into account, with no strong dependence on redshift or luminosity. We derived the high-redshift AGN number counts down to F 0.5−2 keV = 7 × 10 −18 erg cm −2 s −1 , extending previous results to fainter fluxes, especially at z > 4. We put the tightest constraints to date on the low-luminosity end of AGN luminosity function at high redshift. The space-density, in particular, declines at z > 3 at all luminosities, with only a marginally steeper slope for low-luminosity AGN. By comparing the evolution of the AGN and galaxy densities, we suggest that such a decline at high luminosities is mainly driven by the underlying galaxy population, while at low luminosities there are hints of an intrinsic evolution of the parameters driving nuclear activity. Also, the black-hole accretion rate density and star-formation rate density, which are usually found to evolve similarly at z 3, appear to diverge at higher redshifts.

show abstract

“…Since standard stellar population synthesis models do not include nebular emission this may have an impact on the SED fitting and, in particular, on the computed total stellar masses (e.g., Krueger et al 1995;Papaderos et al 1998;Schaerer & de Barros 2009;Atek et al 2011;Curtis-Lake et al 2013;Stark et al 2013;Castellano et al 2014;Santini et al 2015;Pacifici et al 2015). In order to overcome this potential systematic effect for the sample of EELGs, an additional set of fits were computed after removing the contribution of emission line fluxes to the observed broadband magnitudes.…”

Section: The Low Stellar Masses Of Eelgsmentioning

confidence: 99%

Extreme emission-line galaxies out toz~ 1 in zCOSMOS

Amorín

Pérez-Montero

Contini

et al. 2015

A&A

113

View full text Add to dashboard Cite

Context. The study of large and representative samples of low-metallicity star-forming galaxies at different cosmic epochs is of great interest to the detailed understanding of the assembly history and evolution of low-mass galaxies. Aims. We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 ≤ z ≤ 0.93 selected from the 20k zCOSMOS bright survey because of their unusually large emission line equivalent widths. Methods. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging, and optical zCOSMOS spectroscopy to derive the main global properties of star-forming EELGs, such as sizes, stellar masses, star formation rates (SFR), and reliable oxygen abundances using both "direct" and "strong-line" methods. Results. The EELGs are extremely compact (r 50 ∼ 1.3 kpc), low-mass (M * ∼ 10 7 −10 10 M ) galaxies forming stars at unusually high specific star formation rates (sSFR ≡ SFR/M up to 10 −7 yr −1 ) compared to main sequence star-forming galaxies of the same stellar mass and redshift. At rest-frame UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Lyα emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+ log(O/H) = 8.16 ± 0.21 (0.2 Z ) including a handful of extremely metal-deficient (<0.1 Z ) EELGs. While ∼80% of the EELGs show non-axisymmetric morphologies, including clumpy and cometary or tadpole galaxies, we find that ∼29% of them show additional low-surface-brightness features, which strongly suggests recent or ongoing interactions. As star-forming dwarfs in the local Universe, EELGs are most often found in relative isolation. While only very few EELGs belong to compact groups, almost one third of them are found in spectroscopically confirmed loose pairs or triplets. Conclusions. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building up a significant fraction of their present-day stellar mass in an ongoing, galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low-and high-redshift low-mass star-forming galaxies.

show abstract

Stellar Masses From the Candels Survey: The Goods-South and Uds Fields

Cited by 268 publications

References 85 publications

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

High-redshift AGN in the Chandra Deep Fields: the obscured fraction and space density of the sub-L* population

Extreme emission-line galaxies out toz~ 1 in zCOSMOS

Contact Info

Product

Resources

About