ERRATUM: “THE FMOS-COSMOS SURVEY OF STAR-FORMING GALAXIES AT
                    <i>z</i>
                    ∼ 1.6. I. Hα-BASED STAR FORMATION RATES AND DUST EXTINCTION” (2013, ApJL, 777, L8)

Kashino, Daichi; Silverman, John D.; Rodighiero, G.; Renzini, A.; Arimoto, N.; Daddi, E.; Lilly, S. J.; Sanders, D. B.; Kartaltepe, Jeyhan S.; Zahid, H. Jabran; Nagao, Takashi; Sugiyama, Naoshi; Capak, P.; Carollo, C. M.; Chu, J.; Hasinger, G.; Ilbert, O.; Kajisawa, Masaru; Kewley, Lisa J.; Koekemoer, Anton M.; Kovač, K.; Fèvre, O. Le; Masters, D. C.; McCracken, H. J.; Onodera, Makoto; Scoville, N. Z.; Strazzullo, V.; Symeonidis, M.; Taniguchi, Yoshiaki

doi:10.1088/2041-8205/785/2/l37

Cited by 33 publications

(73 citation statements)

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“…More details of this method to estimate AHα is mentioned in subsection 4.1. The Hα emitters in USS1558 show a positive correlation between stellar masses and SFRs, known as the "main sequence" of star-forming galaxies (e.g., Noeske et al 2007;Daddi et al 2007;Kashino et al 2013;Tomczak et al 2016), as already reported in previous studies (Hayashi et al 2012(Hayashi et al , 2016Shimakawa et al 2018).…”

Section: Target Field and Observationsupporting

confidence: 72%

Extended star-forming regions within galaxies in a dense proto-cluster core at z = 2.53

Suzuki

Minowa

Koyama

et al. 2019

Publications of the Astronomical Society of Japan

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At z ∼ 2, star-formation activity is thought to be high even in high-density environments such as galaxy clusters and proto-clusters. One of the critical but outstanding issues is if structural growth of star-forming galaxies can differ depending on their surrounding environments. In order to investigate how galaxies grow their structures and what physical processes are involved in the evolution of galaxies, one requires spatially resolved images of not only stellar components but also star-forming regions within galaxies. We conducted the Adaptive Optics(AO)-assisted imaging observations for star-forming galaxies in a dense proto-cluster core at z = 2.53 with IRCS and AO188 mounted on the Subaru Telescope. A combination of AO and narrow-band filters allows us to obtain resolved maps of Hα-emitting regions with an angular resolution of 0.1-0.2 arcsec, which corresponds to ∼ 1 kpc at z ∼ 2.5. Based on stacking analyses, we compare radial profiles of star-forming regions and stellar components and find that the star-forming region of a sub-sample with log(M * /M ⊙ ) ∼ 10 − 11 is more extended than the stellar component, indicating the inside-out growth of the structure. This trend is similar to the one for star-forming galaxies in general fields at z = 2 − 2.5 obtained with the same observational technique. Our results suggest that the structural evolution of star-forming galaxies at z = 2 − 2.5 is mainly driven by internal secular processes irrespective of surrounding environments.

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Section: Target Field and Observationsupporting

confidence: 72%

Extended star-forming regions within galaxies in a dense proto-cluster core at z = 2.53

Suzuki

Minowa

Koyama

et al. 2019

Publications of the Astronomical Society of Japan

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“…With the deeper magnitude limits, we expect to obtain a lower limit to the BH masses of log M BH ∼ 7.04M ⊙ at z = 2 using the methods detailed in Section 4. Furthermore, the FMOS-COSMOS spectroscopic survey was conducted with the Subaru/FMOS (Kimura et al 2010) NIR high-resolution spectrographs (R ∼ 2200), described in detail in Silverman et al (2015) (see also Kashino et al 2013;Schulze et al 2018). Our sample, therefore, represents the most typical AGN population covering lower luminosities, compared to previous studies at z > 1.…”

Section: Broad-line Agn Sample and Datamentioning

confidence: 98%

No Significant Evolution of Relations between Black Hole Mass and Galaxy Total Stellar Mass Up to z ∼ 2.5

Suh

Civano

Trakhtenbrot

et al. 2020

ApJ

106

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We investigate the cosmic evolution of the ratio between black hole mass (M BH ) and host galaxy total stellar mass (M stellar ) out to z ∼ 2.5 for a sample of 100 X-ray-selected moderate-luminosity, broad-line active galactic nuclei (AGNs) in the Chandra-COSMOS Legacy Survey. By taking advantage of the deep multi-wavelength photometry and spectroscopy in the COSMOS field, we measure in a uniform way the galaxy total stellar mass using a SED decomposition technique and the black hole mass based on broad emission line measurements and single-epoch virial estimates. Our sample of AGN host galaxies has total stellar masses of 10 10−12 M ⊙ , and black hole masses of 10 7.0−9.5 M ⊙ . Combining our sample with the relatively bright AGN samples from the literature, we find no significant evolution of the M BH − M stellar relation with black hole-to-host total stellar mass ratio of M BH /M stellar ∼ 0.3% at all redshifts probed. We conclude that the average black hole-to-host stellar mass ratio appears to be consistent with the local value within the uncertainties, suggesting a lack of evolution of the M BH − M stellar relation up to z ∼ 2.5.

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“…Note that this ratio might be different at high redshifts due to the changing star formation activity and the properties of the ISM of galaxies (e.g., Reddy et al 2015). The literature has not yet arrived at a consensus on this ratio at higher redshifts, although there are indications of an evolution towards unity at z ∼ 2 (Erb et al 2006;Hainline et al 2009;Förster Schreiber et al 2009;Cresci et al 2012;Yabe et al 2012;Kashino et al 2013;Cullen et al 2014;Price et al 2014;Theios et al 2018). Local Figure 5.…”

Section: 23mentioning

confidence: 99%

The Recent Burstiness of Star Formation in Galaxies at z ∼ 4.5 from Hα Measurements

Faisst

Capak

Emami

et al. 2019

ApJ

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The redshift range z = 4 − 6 marks a transition phase between primordial and mature galaxy formation in which galaxies considerably increase their stellar mass, metallicity, and dust content. The study of galaxies in this redshift range is therefore important to understand early galaxy formation and the fate of galaxies at later times. Here, we investigate the burstiness of the recent star-formation history (SFH) of 221 z ∼ 4.5 main-sequence galaxies at log(M/M ) > 9.7 by comparing their ultraviolet (UV) continuum, Hα luminosity, and Hα equivalent-width (EW). The Hα properties are derived from the Spitzer [3.6 µm]−[4.5 µm] broad-band color, thereby properly taking into account model and photometric uncertainties. We find a significant scatter between Hα and UV-derived luminosities and star-formation rates (SFRs). About half of the galaxies show a significant excess in Hα compared to expectations from a constant smooth SFH. We also find a tentative anti-correlation between Hα EW and stellar mass, ranging from 1000Å at log(M/M ) < 10 to below 100Å at log(M/M ) > 11. Consulting models suggests that most z ∼ 4.5 galaxies had a burst of star-formation within the last 50 Myrs, increasing their SFRs by a factor of > 5. The most massive galaxies on the other hand might decrease their SFRs, and may be transitioning to a quiescent stage by z = 4. We identify differential dust attenuation (f ) between stars and nebular regions as the main contributor to the uncertainty. With local galaxies selected by increasing Hα EW (reaching values similar to high-z galaxies), we predict that f approaches unity at z > 4 consistent with the extrapolation of measurements out to z = 2.

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ERRATUM: “THE FMOS-COSMOS SURVEY OF STAR-FORMING GALAXIES AT z ∼ 1.6. I. Hα-BASED STAR FORMATION RATES AND DUST EXTINCTION” (2013, ApJL, 777, L8)

Cited by 33 publications

References 0 publications

Extended star-forming regions within galaxies in a dense proto-cluster core at z = 2.53

Extended star-forming regions within galaxies in a dense proto-cluster core at z = 2.53

No Significant Evolution of Relations between Black Hole Mass and Galaxy Total Stellar Mass Up to z ∼ 2.5

The Recent Burstiness of Star Formation in Galaxies at z ∼ 4.5 from Hα Measurements

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