A Complete 16 μm Selected Galaxy Sample at z ∼ 1: Mid-infrared Spectral Energy Distributions

Huang, Jia-Sheng; Dai, Y. Sophia; Willner, S. P.; Faber, S. M.; Cheng, Cheng; Xu, Hai; Wu, Shengbiao; Shao, Xu; Hao, Cai-Na; Xia, X. Y.; Rigopoulou, D.; Pereira-Santaella, M.; Magdis, G.; Cortzen, Isabella; Yan, Haojing; Fazio, G. G.; Assmann, P.; Araneda, Nicole; Fan, Lulu; Musin, Marat; Wang, Zhenzhu; Kong, Xu; He, Chuan; Esamdin, Ali

doi:10.3847/1538-4357/abec50

Cited by 4 publications

(4 citation statements)

References 135 publications

(200 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We conduct a morphological analysis of a 16 μm PAHselected LIRG-dominated sample from Huang et al (2021) in the three CANDELS fields (GOODS-S, GOODS-N, EGS), and investigate the relations between their morphological and physical properties. Our findings are as follows.…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

A Complete 16 μm Selected Galaxy Sample at z ∼ 1. II. Morphological Analysis

Liang,

Dai 戴,

Huang

et al. 2024

ApJ

Self Cite

View full text Add to dashboard Cite

We present a morphological analysis of the 16 μm flux-density-limited galaxy sample at 0.8 < z < 1.3 from Huang et al. (2021). At the targeted redshift, the 16 μm emission corresponds to the polycyclic aromatic hydrocarbon feature from intense star formation, or dust heated by active galactic nuclei (AGN). Our sample of 479 galaxies are dominated by luminous infrared galaxies (LIRGs; 67%) in three CANDLES fields (Extended Groth Strip, Great Observatories Origins Deep Survey North and South fields), and are further divided into AGN-dominated, star-forming dominated, composite, and blue compact galaxies by their spectral energy distribution types. The majority of our sample (71%) have disk morphologies, with the few AGN-dominated galaxies being more bulge-dominated than the star-forming-dominated and composite galaxies. The distribution of our sample on the Gini versus M 20 plane is consistent with previous studies, where the Sérsic index n shows an increasing trend toward the smaller M 20 and higher Gini region below the dividing line for mergers. The subsample of ultraluminous infrared galaxies (ULIRGs) follows a steep size–mass relation that is closer to the early-type galaxies. In addition, as the 4.5 μm luminosity excess ( L 4.5 exc , proxy for AGN strength) increases, our sample appears to be more bulge dominated (i.e., higher n). Based on the specific star formation rate and compactness ( log 10 Σ 1.5 , Σ 1.5 = M * / R e 1.5 ) diagram, the majority of our LIRG-dominated galaxy sample follows a secular evolution track, and their distribution can be explained without involving any merging activities. Out of the 16 ULIRGs in our sample, six are compact with strong AGN contributions, likely evolving along the fast track from more violent activities.

show abstract

Section: Discussionmentioning

confidence: 99%

“…

We present a morphological analysis of the 16 μm flux-density-limited galaxy sample at 0.8 < z < 1.3 from Huang et al (2021). At the targeted redshift, the 16 μm emission corresponds to the polycyclic aromatic hydrocarbon feature from intense star formation, or dust heated by active galactic nuclei (AGN).

…”

mentioning

confidence: 99%

A Complete 16 μm Selected Galaxy Sample at z ∼ 1. II. Morphological Analysis

Liang,

Dai 戴,

Huang

et al. 2024

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Three systems have X-ray detections with the Chandra X-ray Observatory and presumably contain active galactic nuclei (AGNs). Previous studies have been limited to using spectral-energy-distribution (SED) modeling to separate AGNs and their host galaxies (Burgarella et al 2005;Noll et al 2009;Boquien et al 2019;Huang et al 2021). In contrast, the JWST angular resolution of 0 07-0 14 (= 0.6-1.2 kpc at z = 2) 15 in the NIRcam 2-4.4 μm bands can show a dusty AGN as a point source distinct from the galaxy disk.…”

Section: Introductionmentioning

confidence: 99%

“…The selection criteria, involving 3.6-8.0 μm IRAC colors as well as 24 μm flux density were designed to select star-forming galaxies with strong PAH emission at 1.7  z  2.3 (Huang et al 2004(Huang et al , 2009. Nevertheless, some sample galaxies have an AGN component that produces MIR power-law emission (Huang et al 2021). Most of the sample galaxies were also detected by Herschel in the far-infrared, and some have been detected at submillimeter and millimeter wavelengths.…”

Section: Introductionmentioning

confidence: 99%

A Diverse Population of z ∼ 2 ULIRGs Revealed by JWST Imaging

Huang

Cheng

et al. 2023

ApJ

Self Cite

View full text Add to dashboard Cite

Four ultraluminous infrared galaxies (ULIRGs) observed with JWST/NIRcam in the Cosmos Evolution Early Release Science program offer an unbiased preview of the z ∼ 2 ULIRG population. The objects were originally selected at 24 μm and have strong polycyclic aromatic hydrocarbon emission features observed with Spitzer/Infrared Spectrometer. The four objects have similar stellar masses of ∼1011 M ⊙ but otherwise are quite diverse. One is an isolated disk galaxy, but it has an active nucleus as shown by X-ray observations and by a bright point-source nucleus. Two others are merging pairs with mass ratios of 6–7:1. One has active nuclei in both components, while the other has only one active nucleus: the one in the less-massive neighbor, not the ULIRG. The fourth object is clumpy and irregular and is probably a merger, but there is no sign of an active nucleus. The intrinsic spectral energy distributions for the four active galactic nuclei in these systems are typical of type-2 QSOs. This study is consistent with the idea that even if internal processes can produce large luminosities at z ∼ 2, galaxy merging may still be necessary for the most luminous objects. The diversity of these four initial examples suggests that large samples will be needed to understand the z ∼ 2 ULIRG population.

show abstract

Spectral energy distribution similarity of the local galaxies and the 3.6 μm selected galaxies from the Spitzer Extended Deep Survey

Cheng

Huang

et al. 2021

Res. Astron. Astrophys.

View full text Add to dashboard Cite

The Spitzer Extended Deep Survey (SEDS) as a deep and wide mid-infrared (MIR) survey project provides a sample of 500 000+ sources spreading 1.46 square degree and a depth of 26 AB mag (3σ). Combining with the previous available data, we build a PSF-matched multi-wavelength photometry catalog from u band to 8 μm. We fit the SEDS galaxies spectral energy distributions by the local galaxy templates. The results show that the SEDS galaxy can be fitted well, indicating the high redshift galaxy (z ∼ 1) shares the same templates with the local galaxies. This study would facilitate the further study of the galaxy luminosity and high redshift mass function.

show abstract

A Complete 16 μm Selected Galaxy Sample at z ∼ 1: Mid-infrared Spectral Energy Distributions

Cited by 4 publications

References 135 publications

A Complete 16 μm Selected Galaxy Sample at z ∼ 1. II. Morphological Analysis

A Complete 16 μm Selected Galaxy Sample at z ∼ 1. II. Morphological Analysis

A Diverse Population of z ∼ 2 ULIRGs Revealed by JWST Imaging

Spectral energy distribution similarity of the local galaxies and the 3.6 μm selected galaxies from the Spitzer Extended Deep Survey

Contact Info

Product

Resources

About