INFRARED COLOR SELECTION of MASSIVE GALAXIES at z > 3
Astrophysical Journal, ISSN: 1538-4357, Vol: 816, Issue: 2
2016
- 64Citations
- 33Captures
Metric Options: Counts1 Year3 YearSelecting the 1-year or 3-year option will change the metrics count to percentiles, illustrating how an article or review compares to other articles or reviews within the selected time period in the same journal. Selecting the 1-year option compares the metrics against other articles/reviews that were also published in the same calendar year. Selecting the 3-year option compares the metrics against other articles/reviews that were also published in the same calendar year plus the two years prior.
Example: if you select the 1-year option for an article published in 2019 and a metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019. If you select the 3-year option for the same article published in 2019 and the metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019, 2018 and 2017.
Citation Benchmarking is provided by Scopus and SciVal and is different from the metrics context provided by PlumX Metrics.
Example: if you select the 1-year option for an article published in 2019 and a metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019. If you select the 3-year option for the same article published in 2019 and the metric category shows 90%, that means that the article or review is performing better than 90% of the other articles/reviews published in that journal in 2019, 2018 and 2017.
Citation Benchmarking is provided by Scopus and SciVal and is different from the metrics context provided by PlumX Metrics.
Article Description
We introduce a new color selection technique to identify high-redshift, massive galaxies that are systematically missed by Lyman-break selection. The new selection is based on the H (H) and Infrared Array Camera (IRAC) 4.5 μm bands, specifically mag. These galaxies, called "HIEROs," include two major populations that can be separated with an additional J - H color. The populations are massive and dusty star-forming galaxies at () and extremely dusty galaxies at (). The 350 arcmin of the GOODS-North and GOODS-South fields with the deepest Hubble Space Telescope (HST)/Wide Field Camera 3 (WFC3) near-infrared and IRAC data contain as many as 285 HIEROs down to mag. Inclusion of the most extreme HIEROs, not even detected in the H band, makes this selection particularly complete for the identification of massive high-redshift galaxies. We focus here primarily on () HIEROs, which have a median photometric redshift and stellar mass and are much fainter in the rest-frame UV than similarly massive Lyman-break galaxies (LBGs). Their star formation rates (SFRs), derived from their stacked infrared spectral energy distributions (SEDs), reach ∼240 yr, leading to a specific SFR, Gyr, suggesting that the sSFRs for massive galaxies continue to grow at but at a lower growth rate than from z = 0 to z = 2. With a median half-light radius of 2 kpc, including as compact as quiescent (QS) galaxies at similar redshifts, HIEROs represent perfect star-forming progenitors of the most massive ( ) compact QS galaxies at and have the right number density. HIEROs make up of all galaxies with identified at from their photometric redshifts. This is five times more than LBGs with nearly no overlap between the two populations. While HIEROs make up 15%-25% of the total SFR density at -5, they completely dominate the SFR density taking place in galaxies, and HIEROs are therefore crucial to understanding the very early phase of massive galaxy formation.
Bibliographic Details
http://www.scopus.com/inward/record.url?partnerID=HzOxMe3b&scp=84955318949&origin=inward; http://dx.doi.org/10.3847/0004-637x/816/2/84; https://iopscience.iop.org/article/10.3847/0004-637X/816/2/84; http://stacks.iop.org/0004-637X/816/i=2/a=84?key=crossref.de65bc53c4be897c2957d501b28e45a0; http://stacks.iop.org/0004-637X/816/i=2/a=84/pdf; https://dx.doi.org/10.3847/0004-637x/816/2/84; https://validate.perfdrive.com/9730847aceed30627ebd520e46ee70b2/?ssa=4f9411ff-2b74-4436-a0b6-ff609c729ace&ssb=67963216815&ssc=https%3A%2F%2Fiopscience.iop.org%2Farticle%2F10.3847%2F0004-637X%2F816%2F2%2F84&ssi=4bd6027d-cnvj-40f7-b27f-013840484b32&ssk=botmanager_support@radware.com&ssm=492305926209142977850054840446402157&ssn=f25b5f34c5f6a6f60e998c6d57416dd0029d0900c3c4-8990-4f21-abe47e&sso=b435af8c-bc564dd29dea029c3c5cf592175ca06b4cd01e1a54b10a15&ssp=92989805761726551546172701977699879&ssq=94696838979286082082529239567471940036991&ssr=NTIuMy4yMTcuMjU0&sst=com.plumanalytics&ssu=&ssv=&ssw=&ssx=eyJ1em14IjoiN2Y5MDAwMGMxZDc2YmItMzk2MS00N2VjLTlkZGItNjdmYTVhZTY2ODdlOC0xNzI2NTI5MjM5NDUzNTYwNTUyODg2LTFkZWUzZDE4OWI0MjBjNTI3ODQ3NDciLCJfX3V6bWYiOiI3ZjYwMDBkNzYzNGE3Ni05ZTRkLTRjMmMtYjJhMC1mYzAzNGMyZjE1MjkxNzI2NTI5MjM5NDUzNTYwNTUyODg2LTlmZWQ0ZWZhZTI1MTVkZjE3ODQ4MzQiLCJyZCI6ImlvcC5vcmcifQ==
American Astronomical Society
Provide Feedback
Have ideas for a new metric? Would you like to see something else here?Let us know