Exploring the Evolution of Star Formation and Dwarf Galaxy Properties with JWST/MIRI Serendipitous Spectroscopic Surveys

Bonato, M.; Sajina, Anna; Zotti, G. de; McKinney, Jed; Baronchelli, Ivano; Negrello, M.; Marchesini, Danilo; Roebuck, Eric J.; Shipley, Heath; Kurinsky, Noah; Pope, Alexandra; Noriega-Crespo, A.; Yan, Lin; Kirkpatrick, Allison

doi:10.3847/1538-4357/aa5c85

Cited by 5 publications

(9 citation statements)

References 127 publications

(239 reference statements)

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“…This was done by coupling relationships between line and IR continuum luminosity (or bolometric luminosity in the case of AGNs) with the SFR and luminosity functions by Cai et al (2013), which accurately match the observational data. We have adopted the relationships found by Bonato et al (2014aBonato et al ( ,b, 2015Bonato et al ( , 2017b for the SF contribution to the emission of 22 IR fine-structure lines and 6 PAH lines, and for the AGN emission of 27 IR lines. For the SF contribution of 3 lines, the relationships were recalibrated using new data, and new relationships were determined for 10 CO lines, for the SF contribution to 3 lines, and for the AGN contribution to 5 lines.…”

Section: Discussionmentioning

confidence: 99%

“…To estimate the number of AGN and galaxy line detections achievable with OST/OSS surveys, we coupled the SFR/IR luminosity functions (for the galaxies) or the bolometric luminosity functions (for the AGNs) of each population, as given by the model, with relationships between line and IR 4 or bolometric luminosities. We used the calibrations derived by Bonato et al (2014aBonato et al ( ,b, 2015Bonato et al ( , 2017b for 31 IR fine-structure lines and the 6 polycyclic aromatic hydrocarbon (PAH) bands at 3.3, 6.2, 7.7, 8.6, 11.3 and 12.7 µm, as they will be accessible in the OST/OSS wavelength range.…”

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

“…Note that while the AGN contribution to the high-J CO lines could be significant, the available observational data are not sufficient to support a derivation of the empirical correlation between AGN bolometric and CO line luminosity. Similarly to what was done in Bonato et al (2017b), the detection limits for the broad PAH bands were computed assuming that the spectra are degraded to R = 50 from the original R = 300, resulting in a sensitivity gain by a factor of √ 6.…”

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

“…We used the calibrations derived by Bonato et al (2014aBonato et al ( ,b, 2015Bonato et al ( , 2017b for 31 IR fine-structure lines and the 6 PAH bands at 3. 3, 6.2, 7.7, 8.6, 11.3, and 12.7 µm, as they will be accessible in the OST/OSS wavelength range.…”

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

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Origins Space Telescope: Predictions for far-IR spectroscopic surveys

Bonato

Zotti

Leisawitz

et al. 2019

Publ. Astron. Soc. Aust.

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We illustrate the extraordinary potential of the (far-IR) Origins Survey Spectrometer (OSS) on board the Origins Space Telescope (OST) to address a variety of open issues on the co-evolution of galaxies and AGNs. We present predictions for blind surveys, each of 1000 h, with different mapped areas (a shallow survey covering an area of 10 deg 2 and a deep survey of 1 deg 2 ) and two different concepts of the OST/OSS: with a 5.9 m telescope (Concept 2, our reference configuration) and with a 9.1 m telescope (Concept 1, previous configuration). In 1000 h, surveys with the reference concept will detect from ∼ 1.9 × 10 6 to ∼ 8.7 × 10 6 lines from ∼ 4.8 × 10 5 -2.7 × 10 6 star-forming galaxies and from ∼ 1.4 × 10 4 to ∼ 3.8 × 10 4 lines from ∼ 1.3 × 10 4 -3.5 × 10 4 AGNs. The shallow survey will detect substantially more sources than the deep one; the advantage of the latter in pushing detections to lower luminosities/higher redshifts turns out to be quite limited. The OST/OSS will reach, in the same observing time, line fluxes more than one order of magnitude fainter than the SPICA/SMI and will cover a much broader redshift range. In particular it will detect tens of thousands of galaxies at z ≥ 5, beyond the reach of that instrument. The polycyclic aromatic hydrocarbons lines are potentially bright enough to allow the detection of hundreds of thousands of star-forming galaxies up to z ∼ 8.5, i.e. all the way through the re-ionization epoch. The proposed surveys will allow us to explore the galaxy-AGN co-evolution up to z ∼ 5.5 − 6 with very good statistics. OST Concept 1 does not offer significant advantages for the scientific goals presented here.

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Section: Discussionmentioning

confidence: 99%

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

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Origins Space Telescope: Predictions for far-IR spectroscopic surveys

Bonato

Zotti

Leisawitz

et al. 2019

Publ. Astron. Soc. Aust.

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“…The medium-resolution spectrometer (Wells et al 2015), which is part of the Mid-Infrared Instrument (MIRI) on JWST, will enable separation of PAH emission from continuum in the same manner, but with higher resolution and on smaller spatial scales within host galaxies. It will also enable detection of high-ionization gas lines excited by the AGN (Bonato et al 2017), further improving our ability to detect and measure the physical properties (such as accretion rates and Eddington ratios) of dust-obscured black holes.…”

Section: Introductionmentioning

confidence: 99%

The AGN–Star Formation Connection: Future Prospects with JWST

Kirkpatrick¹,

Alberts

Pope

et al. 2017

ApJ

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The bulk of the stellar growth over cosmic time is dominated by IR-luminous galaxies at cosmic noon ( = -z 1 2), many of which harbor a hidden active galactic nucleus (AGN). We use state-of-the-art infrared color diagnostics, combining Spitzer and Herschel observations, to separate dust-obscured AGNs from dusty star-forming galaxies (SFGs) in the CANDELS and COSMOS surveys. We calculate 24 μm counts of SFGs, AGN/star-forming "Composites," and AGNs. AGNs and Composites dominate the counts above 0.8 mJy at 24 μm, and Composites form at least 25% of an IR sample even to faint detection limits. We develop methods to use the Mid-Infrared Instrument (MIRI) on JWST to identify dust-obscured AGNs and Composite galaxies from~-z 1 2. With the sensitivity and spacing of MIRI filters, we will detect >4 times as many AGN hosts as with Spitzer/IRAC criteria. Any star formation rates based on the 7.7 μm PAH feature (likely to be applied to MIRI photometry) must be corrected for the contribution of the AGN, or the star formation rate will be overestimated by ∼35% for cases where the AGN provides half the IR luminosity and ∼50% when the AGN accounts for 90% of the luminosity. Finally, we demonstrate that our MIRI color technique can select AGNs with an Eddington ratio of l~0.01 Edd and will identify AGN hosts with a higher specific star formation rate than X-ray techniques alone. JWST/MIRI will enable critical steps forward in identifying and understanding dust-obscured AGNs and the link to their host galaxies.

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JWST/MIRI Simulated Imaging: Insights into Obscured Star Formation and AGNs for Distant Galaxies in Deep Surveys

Yang

Papovich

Bagley

et al. 2021

ApJ

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The James Webb Space Telescope MIRI instrument will revolutionize extragalactic astronomy with unprecedented sensitivity and angular resolution in mid-IR. Here we assess the potential of MIRI photometry to constrain galaxy properties in the Cosmic Evolution Early Release Science (CEERS) survey. We derive estimated MIRI fluxes from the spectral energy distributions (SEDs) of real sources that fall in a planned MIRI pointing. We also obtain MIRI fluxes for hypothetical active galactic nucleus (AGN)–galaxy mixed models varying the AGN fractional contribution to the total IR luminosity (fracAGN). Based on these model fluxes, we simulate CEERS imaging (3.6 hr exposure) in six bands from F770W to F2100W using mirisim and reduce these data using jwst pipeline. We perform point-spread-function-matched photometry with tphot and fit the source SEDs with x-cigale, simultaneously modeling photometric redshift and other physical properties. Adding the MIRI data, the accuracy of both redshift and fracAGN is generally improved by factors of ≳2 for all sources at z ≲ 3. Notably, for pure-galaxy inputs (fracAGN = 0), the accuracy of fracAGN is improved by ∼100 times thanks to MIRI. The simulated CEERS MIRI data are slightly more sensitive to AGN detections than the deepest X-ray survey, based on the empirical L X–L 6 μm relation. Like X-ray observations, MIRI can also be used to constrain the AGN accretion power (accuracy ≈0.3 dex). Our work demonstrates that MIRI will be able to place strong constraints on the mid-IR luminosities from star formation and AGNs and thereby facilitate studies of the galaxy/AGN coevolution.

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Exploring the Evolution of Star Formation and Dwarf Galaxy Properties with JWST/MIRI Serendipitous Spectroscopic Surveys

Cited by 5 publications

References 127 publications

Origins Space Telescope: Predictions for far-IR spectroscopic surveys

Origins Space Telescope: Predictions for far-IR spectroscopic surveys

The AGN–Star Formation Connection: Future Prospects with JWST

JWST/MIRI Simulated Imaging: Insights into Obscured Star Formation and AGNs for Distant Galaxies in Deep Surveys

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