Response to the letter to the editor by M. Elsner <i>et al</i>: “Comment on Binhai Ren <i>et al</i> (2013;15:28–41). Long term reversal of diabetes in non‐obese diabetic mice by liver‐directed gene therapy”

Simpson, Ann M.; Ren, Bin; O’Brien, Bronwyn A.; Nassif, Najah T.

doi:10.1002/jgm.2724

Cited by 26 publications

(71 citation statements)

References 5 publications

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“…At z 1 SMGs may contribute up to 50 percent of the star-formation rate density (e.g., Peacock et al 2000;Chapman et al 2005;Barger et al 2012;Swinbank et al 2014;Casey, Narayanan & Cooray 2014;Zavala et al 2017). SMGs at higher redshifts (z 3) may also hold the key to explaining the populations of z ∼ 2-3 compact, quiescent galaxies now being detected (e.g., Toft et al 2014;Hodge et al 2016;Simpson et al 2017b). The high stellar masses and apparent old ages of these galaxies suggest that they formed in rapid, intense bursts of star formation at z > 3 (e.g., Glazebrook et al 2017;Simpson et al 2017b).…”

Section: Introductionmentioning

confidence: 99%

“…SMGs at higher redshifts (z 3) may also hold the key to explaining the populations of z ∼ 2-3 compact, quiescent galaxies now being detected (e.g., Toft et al 2014;Hodge et al 2016;Simpson et al 2017b). The high stellar masses and apparent old ages of these galaxies suggest that they formed in rapid, intense bursts of star formation at z > 3 (e.g., Glazebrook et al 2017;Simpson et al 2017b). Such starbursts may be linked to high redshift SMGs, meaning these galaxies are an essential element in models of massive galaxy formation.…”

Section: Introductionmentioning

confidence: 99%

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An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Identifying Candidate z ∼ 4.5 [C II] Emitters

Cooke

Smail

Swinbank

et al. 2018

ApJ

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We report the results of a search for serendipitous [C II] 157.74 µm emitters at z ≃ 4.4-4.7 using the Atacama Large Millimeter/submillimeter Array (ALMA). The search exploits the AS2UDS continuum survey, which covers ∼ 50 arcmin 2 of the sky towards 695 luminous (S 870 1 mJy) submillimeter galaxies (SMGs), selected from the SCUBA-2 Cosmology Legacy Survey (S2CLS) 0.96 deg 2 Ultra Deep Survey (UDS) field. We detect ten candidate line emitters, with an expected false detection rate of ten percent. All of these line emitters correspond to 870 µm continuum-detected sources in AS2UDS. The emission lines in two emitters appear to be high-J CO, but the remainder have multiwavelength properties consistent with [C II] from z ≃ 4.5 galaxies. Using our sample, we place a lower limit of > 5 × 10 −6 Mpc −3 on the space density of luminous (L IR ≃ 10 13 L ⊙ ) SMGs at z = 4.40-4.66, suggesting ≥ 7 percent of SMGs with S 870µm 1 mJy lie at 4 < z < 5. From stacking the highresolution (∼ 0.15 ′′ full-width half maximum) ALMA 870 µm imaging, we show that the [C II] line emission is more extended than the continuum dust emission, with an average effective radius for the [C II] of r e = 1.7 +0.1 −0.2 kpc compared to r e = 1.0 ± 0.1 kpc for the continuum (rest-frame 160 µm). By fitting the far-infrared photometry for these galaxies from 100-870 µm, we show that SMGs at z ∼ 4.5 have a median dust temperature of T d = 55 ± 4 K. This is systematically warmer than 870 µm-selected SMGs at z ≃ 2, which typically have temperatures around 35 K. These z ≃ 4.5 SMGs display a steeper trend in the luminosity-temperature plane than z ≤ 2 SMGs. We discuss the implications of this result in terms of the selection biases of high redshift starbursts in far-infrared/submillimeter surveys.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Identifying Candidate z ∼ 4.5 [C II] Emitters

Cooke

Smail

Swinbank

et al. 2018

ApJ

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“…Multiplicity fractions (defined as the fraction of total sources which resolve into multiple components) appear to range between 10 per cent (Chen et al 2013) and 50 per cent (Hodge et al 2013), with other studies finding values within that range (e.g., Barger et al 2012;Hezaveh et al 2013, measuring 25 per cent and > 20 per cent fractions respectively) 2 . This variation is likely due in part to different sample selection between studies, which select their targets based on flux measurements based anywhere between 450-µm (e.g., Chen et al 2013) and 1.2 mm (e.g., Hezaveh et al 2013), though largely the systems are selected close to 850-µm (Hodge et al 2013;Karim et al 2013;Simpson et al 2015). Another possible source of variation is the indication that the multiplicity fraction may be dependent on the FIR flux observed, with brighter sources more likely to have multiple components (Karim et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The multiplicity of 250-μmHerschelsources in the COSMOS field

Scudder

Oliver

Hurley

et al. 2016

Mon. Not. R. Astron. Soc.

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details.

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“…Coppin et al 2008;Simpson et al 2012). However, given the combination of the implied high levels of obscuration and relatively short QSO lifetimes of ∼20-40 Myr (Martini & Weinberg 2001;Goncalves, Steidel & Pettini 2008), it has been difficult to select and confirm large samples of youthful QSOs.…”

Section: Introductionmentioning

confidence: 99%

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

Violino¹,

Coppin²,

Stevens³

et al. 2016

Mon. Not. R. Astron. Soc.

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It is thought that a class of broad absorption line (BAL) QSOs, characterised by Fe absorption features in their UV spectra (called 'FeLoBALs'), could mark a transition stage between the end of an obscured starburst event and a youthful QSO beginning to shed its dust cocoon, where Fe has been injected into the interstellar medium by the starburst. To test this hypothesis we have undertaken deep SCUBA-2 850 µm observations of a sample of 17 FeLoBAL QSOs with 0.89 z 2.78 and -23.31 M B -28.50 to directly detect an excess in the thermal emission of the dust which would probe enhanced star-formation activity. We find that FeLoBALs are not luminous sources in the submillimetre, none of them are individually detected at 850 µm, nor as a population through stacking (F s = 1.14 ± 0.58 mJy). Statistical and survival analyses reveal that FeLoBALs have sub-mm properties consistent with BAL and non-BAL QSOs with matched redshifts and magnitudes. An SED fitting analysis shows that the FIR emission is dominated by AGN activity, and a starburst component is required only in 6/17 sources of our sample; moreover the integrated total luminosity of 16/17 sources is L 10 12 L , high enough to classify FeLoBALs as infrared luminous.In conclusion, we do not find any evidence in support of FeLoBAL QSOs being a transition population between a ULIRG and an unobscured QSO; in particular, FeLoBALs are not characterized by a cold starburst which would support this hypothesis.

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Response to the letter to the editor by M. Elsner et al: “Comment on Binhai Ren et al (2013;15:28–41). Long term reversal of diabetes in non‐obese diabetic mice by liver‐directed gene therapy”

Cited by 26 publications

References 5 publications

An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Identifying Candidate z ∼ 4.5 [C II] Emitters

An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Identifying Candidate z ∼ 4.5 [C II] Emitters

The multiplicity of 250-μmHerschelsources in the COSMOS field

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

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