Women and Educational Administration

McLure, Gail T.; McLure, John W.

doi:10.1002/j.2164-6163.1976.tb00206.x

Cited by 9 publications

(18 citation statements)

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“…Fourthly, it is also clear that the objects which remain on the local relation, even out to the highest redshifts, are star‐forming discs, with the passive galaxies, including the passive disc components, confined to the more compact population. This result mirrors that recently reported by McLure et al () who found, for spectroscopically confirmed galaxies of comparably high mass at z ≃ 1.4, that all objects with low sSFR (i.e. sSFR < 10 −10 Gyr −1 ) lie below the present‐day size–mass relation, irrespective of morphological classification.…”

Section: Discussionsupporting

confidence: 91%

“…Moreover, several local studies have now clarified the relative dearth of comparably compact systems surviving to the present day (Trujillo et al ; Taylor et al ), strengthening the argument that the compact high‐redshift systems must undergo a period of significant size evolution with limited mass growth in order to reach the local galaxy size–mass relation by z = 0 (e.g. McLure et al ).…”

Section: Introductionmentioning

confidence: 91%

“…The effects of including ‘double burst models’ in the SED fitting have been explored by Michałowski et al () and McLure et al (). However, while Michałowski et al () show that two‐component models can produce significantly larger stellar masses than single‐component models for extreme starbursting objects such as submillimetre galaxies, McLure et al () report that the mass difference is relatively small for more typical z ≃ 1–2 galaxies (〈Δ M * 〉 ≃ 0.1 dex), presumably because an exponentially decaying star formation history provides a reasonable description of reality for most massive galaxies at these epochs. Accordingly, for the present study we decided to adopt the stellar mass estimates obtained with the BC03 tau‐models, in order to most easily facilitate direct comparison with previous studies.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

“…All of these scenarios can potentially induce sufficient size growth, but there are problems with some of the accompanying predictions of these growth mechanisms. For the major‐merger scenario these include reconciling the number of major mergers required to facilitate the required size growth with the number of major mergers expected since z ∼ 1 from N ‐body simulations (Hopkins et al ), and the disparity between the inferred large mass growth of these (already massive) systems and the latest estimates of the local galaxy stellar mass function (Baldry et al ; McLure et al ). These problems, coupled with results from numerical simulations, which show that AGN‐driven expansion occurs when the galaxy is much younger than the typical ages of high‐redshift compact objects (>0.5 Gyr) (Ragone‐Figueroa & Granato ), have now led most researchers to conclude in favour of a picture in which most size growth since z ≃ 2 is driven by minor gas‐poor mergers in the outer regions of galaxies, building up stellar haloes around compact cores, with (relatively) small overall mass growth (Bezanson et al ; Naab, Johansson & Ostriker ; Hopkins et al ; van Dokkum et al ; McLure et al ; Trujillo, Carrasco & Ferré‐Mateu ).…”

Section: Introductionmentioning

confidence: 99%

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The morphologies of massive galaxies at 1 <z< 3 in the CANDELS-UDS field: compact bulges, and the rise and fall of massive discs

Bruce

Dunlop

Cirasuolo

et al. 2012

Monthly Notices of the Royal Astronomical Society

155

208

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We have used high‐resolution, Hubble Space Telescope, near‐infrared imaging to conduct a detailed analysis of the morphological properties of the most massive galaxies at high redshift, modelling the WFC3/IR H160‐band images of the ≃200 galaxies in the CANDELS‐UDS field with photometric redshifts 1 < z < 3, and stellar masses M* > 1011 M⊙. We have explored the results of fitting single‐Sérsic and bulge+disc models, and have investigated the additional errors and potential biases introduced by uncertainties in the background and the on‐image point spread function. This approach has enabled us to obtain formally acceptable model fits to the WFC3/IR images of >90 per cent of the galaxies. Our results indicate that these massive galaxies at 1 < z < 3 lie both on and below the local size–mass relation, with a median effective radius of ∼2.6 kpc, a factor of ≃2.3 smaller than comparably massive local galaxies. Moreover, we find that bulge‐dominated objects in particular show evidence for a growing bimodality in the size–mass relation with increasing redshift, and by z > 2 the compact bulges display effective radii a factor of ≃4 smaller than local ellipticals of comparable mass. These trends also appear to extend to the bulge components of disc‐dominated galaxies. In addition, we find that, while such massive galaxies at low redshift are generally bulge‐dominated, at redshifts 1 < z < 2 they are predominantly mixed bulge+disc systems, and by z > 2 they are mostly disc‐dominated. The majority of the disc‐dominated galaxies are actively forming stars, although this is also true for many of the bulge‐dominated systems. Interestingly, however, while most of the quiescent galaxies are bulge‐dominated, we find that a significant fraction (25–40 per cent) of the most quiescent galaxies, with specific star formation rates sSFR < 10−10 yr−1, have disc‐dominated morphologies. Thus, while our results show that the massive galaxy population is undergoing dramatic changes at this crucial epoch, they also suggest that the physical mechanisms which quench star formation activity are not simply connected to those responsible for the morphological transformation of massive galaxies into present‐day giant ellipticals.

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Section: Discussionsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 91%

Section: Data and Sample Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The morphologies of massive galaxies at 1 <z< 3 in the CANDELS-UDS field: compact bulges, and the rise and fall of massive discs

Bruce

Dunlop

Cirasuolo

et al. 2012

Monthly Notices of the Royal Astronomical Society

155

208

View full text Add to dashboard Cite

show abstract

“…Finally, we note that the sSFR ≳ 10–100 Gyr −1 obtained here for the LAEs is significantly larger than the typical value of ∼2–3 Gyr −1 found for LBGs by other authors at z ∼ 2 and at redshifts up to z > 6 (see e.g. Daddi et al 2007; Stark et al 2009; González et al 2010; McLure et al 2011). However, some LBGs at z ∼ 2–3 (Erb et al 2006b,c; Yoshikawa et al 2010; Dessauges‐Zavadsky et al 2011), some LAEs at z ∼ 3–4 (Ono et al 2010) and some LBGs at z ≳ 4 (Schaerer & de Barros 2010; de Barros et al, in preparation) also show comparably high sSFR (and a large scatter).…”

Section: Sed Fittingcontrasting

confidence: 69%

The properties of the brightest Lyα emitters at ★

Lidman¹,

Hayes²,

Jones³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We use deep Very Large Telescope (VLT) optical and near‐infrared spectroscopy and deep Spitzer/IRAC imaging to examine the properties of two of the most luminous Lyα emitters at z= 5.7. The continuum redward of the Lyα line is clearly detected in both objects, thus facilitating a relatively accurate measurement (10–20 per cent uncertainties) of the observed rest‐frame equivalent widths, which are around 160 Å for both objects. Through detailed modelling of the profile of the Lyα line with a 3D Monte Carlo radiative transfer code, we estimate the intrinsic rest‐frame equivalent width of Lyα and find values that are around 300 Å, which is at the upper end of the range allowed for very young, moderately metal‐poor star‐forming galaxies. However, the uncertainties are large and values as high as 700 Å are permitted by the data. Both Lyα emitters are detected at 3.6 m in deep images taken with the Spitzer Space Telescope. We use these measurements, the measurement of the continuum redward of Lyα and other photometry to constrain the spectral energy distributions of these very luminous Lyα emitters and to compare them with three similar Lyα emitters from the literature. The contribution from nebular emission is included in our models: excluding it results in significantly higher masses. Four of the five Lyα emitters have masses of the order of ∼109 M⊙ and fairly high specific star formation rates (≳10–100 Gyr−1). While our two Lyα emitters appear similar in terms of the observed Lyα rest‐frame equivalent width, they are quite distinct from each other in terms of age, mass and star formation history. Evidence for dust is found in all objects, and emission from nebular lines often makes a dominant contribution to the rest‐frame 3.6 m flux. Rich in emission lines, these objects are prime targets for the next generation of extremely large telescopes, the James Webb Space Telescope (JWST) and the Atacama Large Millimeter Array (ALMA).

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The Hubble Space Telescope colours of high-redshift Population III galaxies with strong Lyα emission

Zackrisson¹,

Inoue²,

Rydberg³

et al. 2011

Monthly Notices of the Royal Astronomical Society: Letters

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Population III (pop III) galaxies, made partly or exclusively of metal-free stars, are predicted to exist at high redshifts and may produce very strong Lyα emission. A substantial fraction of these Lyα photons are likely absorbed in the intergalactic medium at z > 6, but recent simulations suggest that significant Lyα emission may be detectable up to z ≈ 8.5, i.e. well into the reionization epoch. Here, we argue that high-redshift pop III galaxies with strong Lyα emission can be identified in Hubble Space Telescope imaging data because of their unusual colours. We quantify this effect in some of the filters used in Y-band dropout searches for galaxies at z ≈ 8 and find that pop III galaxies with high Lyα fluxes may exhibit much bluer J − H colours at z ≈ 8-10 than any normal type of galaxy at these redshifts. This colour signature can arise even if pop III stars account for as little as ∼10 −3 to 10 −2 of the stellar mass in these galaxies. Some of the anomalously blue objects reported in current Y-band dropout samples do in fact meet the colour criteria for Lyα-emitting pop III galaxies.

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Women and Educational Administration

Cited by 9 publications

References 0 publications

The morphologies of massive galaxies at 1 <z< 3 in the CANDELS-UDS field: compact bulges, and the rise and fall of massive discs

The morphologies of massive galaxies at 1 <z< 3 in the CANDELS-UDS field: compact bulges, and the rise and fall of massive discs

The properties of the brightest Lyα emitters at ★

The Hubble Space Telescope colours of high-redshift Population III galaxies with strong Lyα emission

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