Probing the Baryon Cycle of Galaxies with <i>SPICA</i> Mid- and Far-Infrared Observations

Tak, F. F. S. van der; Madden, S.; Roelfsema, Peter; Armus, L.; Baes, M.; Bernard─Salas, J.; Bolatto, Alberto D.; Bontemps, Sylvain; Bot, Caroline; Bradford, C. M.; Braine, J.; Ciesla, L.; Clements, D. L.; Cormier, D.; Fernández-Ontiveros, J. A.; Galliano, F.; Giard, M.; Gomez, Haley Louise; González-Alfonso, E.; Herpin, Fabrice; Johnstone, Doug; Jones, A. P.; Kaneda, Hidehiro; Kemper, F.; Lebouteiller, V.; Matsuura, M.; Onaka, Takashi; Pérez‐González, P. G.; Shipman, Russ; Spinoglio, L.

doi:10.1017/pasa.2017.67

Cited by 13 publications

(14 citation statements)

References 183 publications

(265 reference statements)

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“…This can enable, for example, studies of circumnuclear star formation out to z ≈ 0.8. On a longer timescale, the superior sensitivity of the Space Infrared Telescope for Cosmology and Astrophysics (SPICA; Swinyard et al 2009;Egami et al 2018;Roelfsema et al 2018;van der Tak et al 2018) promises even greater reach to the early Universe. For instance, the instantaneous wavelength coverage of 34-230 µm by the SPICA Far Infrared Instrument (SAFARI) in principle can detect the rest-frame mid-IR neon lines in the first-generation galaxies and AGNs.…”

Section: Future Applicationsmentioning

confidence: 99%

A New Method to Measure Star Formation Rates in Active Galaxies Using Mid-infrared Neon Emission Lines

Zhuang

Shangguan

2019

ApJ

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The star formation rate (SFR) is one of the most fundamental parameters of galaxies, but nearly all of the standard SFR diagnostics are difficult to measure in active galaxies because of contamination from the active galactic nucleus (AGN). Being less sensitive to dust extinction, the mid-infrared fine-structure lines of [Ne II] 12.81 µm and [Ne III] 15.56 µm effectively trace the SFR in star-forming galaxies. These lines also have the potential to serve as a reliable SFR indicator in active galaxies, provided that their contribution from the AGN narrow-line region can be removed. We use a new set of photoionization calculations with realistic AGN spectral energy distributions and input assumptions to constrain the magnitude of [Ne II] and [Ne III] produced by the narrow-line region for a given strength of [Ne V] 14.32 µm. We demonstrate that AGNs emit a relatively restricted range of [Ne II]/[Ne V] and [Ne III]/[Ne V] ratios. Hence, once [Ne V] is measured, the AGN contribution to the low-ionization Ne lines can be estimated, and the SFR can be determined from the strength of [Ne II] and [Ne III].We find that AGN host galaxies have similar properties as compact extragalactic H II regions, which indicates that the star formation in AGN hosts is spatially concentrated. This suggests a close relationship between black hole accretion and nuclear star formation. We update the calibration of [Ne II] and [Ne III] strength as a SFR indicator, explicitly considering the effects of metallicity, finding very good relations between Ne fractional abundances and the [Ne III]/[Ne II] ratio for different metallicities, ionization parameters, and starburst ages. Comparison of neon-based SFRs with independent SFRs for active and star-forming galaxies shows excellent consistency with small scatter (∼ 0.18 dex).

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Section: Future Applicationsmentioning

confidence: 99%

A New Method to Measure Star Formation Rates in Active Galaxies Using Mid-infrared Neon Emission Lines

Zhuang

Shangguan

2019

ApJ

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“…aqueous alteration), as well as CO 2 ice and molecules like C 2 H 2 and fullerenes. A table listing these various spectral tracers can be found in van der Tak et al (2017). .…”

Section: The Power Of Infrared Diagnosticsmentioning

confidence: 99%

“…These questions, their background science, and how SPICA would help resolve them, are discussed in much more detail in a dedicated series of papers (Spinoglio et al 2017;Fernández-Ontiveros et al 2017;González-Alfonso et al 2017;Gruppioni et al 2017;Kaneda et al 2017;E. Egami et al, in preparation;van der Tak et al 2017;P. André, in preparation;Trapman et al 2017;Notsu et al 2017Notsu et al , 2016; I. Kamp 2018).…”

Section: The Power Of Infrared Diagnosticsmentioning

confidence: 99%

“…Dole et al 2006). Observations at IR wavelengths are optimal for the study of galactic evolution in which peak activity occurs at redshifts of z ∼1-4, when the Universe was roughly 2-3-Gyr old-as was concluded primarily through deep and wide-field observations with previous infrared space observatories: IRAS (Neugebauer et al 1984), ISO (Kessler et al 1996), Spitzer (Werner et al 2004), AKARI (Murakami et al 2007), Herschel (Pilbratt et al 2010), and WISE (Wright et al 2010). In addition, many of the basic processes of star formation and evolution, from pre-stellar cores to the clearing of gaseous protoplanetary discs, and the presence of dust excess around main-sequence stars, were discovered by these pioneering missions.…”

Section: Introductionmentioning

confidence: 96%

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SPICA—A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Roelfsema

Shibai

Armus

et al. 2018

Publ. Astron. Soc. Aust.

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102

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Measurements in the infrared wavelength domain allow us to assess directly the physical state and energy balance of cool matter in space, thus enabling the detailed study of the various processes that govern the formation and early evolution of stars and planetary systems in the Milky Way and of galaxies over cosmic time. Previous infrared missions, from IRAS to Herschel, have revealed a great deal about the obscured Universe, but sensitivity has been limited because up to now it has not been possible to fly a telescope that is both large and cold. Such a facility is essential to address key astrophysical questions, especially concerning galaxy evolution and the development of planetary systems.SPICA is a mission concept aimed at taking the next step in mid-and far-infrared observational capability by combining a large and cold telescope with instruments employing state-of-the-art ultrasensitive detectors. The mission concept foresees a 2.5-meter diameter telescope cooled to below 8 K. Rather than using liquid cryogen, a combination of passive cooling and mechanical coolers will be used to cool both the telescope and the instruments. With cooling not dependent on a limited cryogen supply, the mission lifetime can extend significantly beyond the required three years. The combination of low telescope background and instruments with state-of-the-art detectors means that SPICA can provide a huge advance on the capabilities of previous missions.The SPICA instrument complement offers spectral resolving power ranging from R ∼50 through 11000 in the 17-230 µm domain as well as R ∼28.000 spectroscopy between 12 and 18 µm. Additionally SPICA will be capable of efficient 30-37 µm broad band mapping, and small field spectroscopic and polarimetric imaging in the 100-350 µm range. SPICA will enable far infrared spectroscopy with an unprecedented sensitivity of ∼ 5 × 10 −20 W/m 2 (5σ/1hr) -at least two orders of magnitude improvement over what has been attained to date. With this exceptional leap in performance, new domains in infrared astronomy will become accessible, allowing us, for example, to unravel definitively galaxy evolution and metal production over cosmic time, to study dust formation and evolution from very early epochs onwards, and to trace the formation history of planetary systems.

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“…As has been demonstrated by the large body of work with ISO and Spitzer, as reviewed by Genzel & Cesarsky (2000) and Soifer, Helou, & Werner (2008), respectively, the rest-frame mid-infrared spectral range is extremely rich in diagnostic information, with a variety of atomic fine-structure lines, molecular hydrogen (H 2 ) lines, PAH features, and silicate emission/absorption features [e.g., see Genzel et al (1998) for ISO and Armus et al (2007) for Spitzer results, as well as the companion papers by Spinoglio et al (2017) and Van der Tak et al (2018)]. Some galaxies are so embedded in dust that rest-frame mid-infrared spectroscopy is crucial for identifying the dominant luminosity source (whether star formation or AGN).…”

Section: Probing the Z > 5 Universementioning

confidence: 99%

Probing the high-redshift universe with SPICA: Toward the epoch of reionisation and beyond

Egami

Gallerani

Schneider

et al. 2018

Publ. Astron. Soc. Aust.

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With the recent discovery of a dozen dusty star-forming galaxies and around 30 quasars at z > 5 that are hyper-luminous in the infrared (µ L IR > 10 13 L , where µ is a lensing magnification factor), the possibility has opened up for SPICA, the proposed ESA M5 mid-/far-infrared mission, to extend its spectroscopic studies toward the epoch of reionization and beyond. In this paper, we examine the feasibility and scientific potential of such observations with SPICA's far-infrared spectrometer SAFARI, which will probe a spectral range (35-230 µm) that will be unexplored by ALMA and JWST. Our simulations show that SAFARI is capable of delivering good-quality spectra for hyper-luminous infrared galaxies (HyLIRGs) at z = 5-10, allowing us to sample spectral features in the rest-frame mid-infrared and to investigate a host of key scientific issues, such as the relative importance of star formation versus AGN, the hardness of the radiation field, the level of chemical enrichment, and the properties of the molecular gas. From a broader perspective, SAFARI offers the potential to open up a new frontier in the study of the early Universe, providing access to uniquely powerful spectral features for probing first-generation objects, such as the key cooling lines of low-metallicity or metal-free forming galaxies (fine-structure and H2 lines) and emission features of solid compounds freshly synthesized by Population III supernovae. Ultimately, SAFARI's ability to explore the high-redshift Universe will be determined by the availability of sufficiently bright targets (whether intrinsically luminous or gravitationally lensed). With its launch expected around 2030, SPICA is ideally positioned to take full advantage of upcoming wide-field surveys such as LSST, SKA, Euclid, and WFIRST, which are likely to provide extraordinary targets for SAFARI.1 Some other SPICA papers refer to this POL field of view as 80 ×80 , but it is 160 ×160 according to the latest design.

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Probing the Baryon Cycle of Galaxies with SPICA Mid- and Far-Infrared Observations

Cited by 13 publications

References 183 publications

A New Method to Measure Star Formation Rates in Active Galaxies Using Mid-infrared Neon Emission Lines

A New Method to Measure Star Formation Rates in Active Galaxies Using Mid-infrared Neon Emission Lines

SPICA—A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Probing the high-redshift universe with SPICA: Toward the epoch of reionisation and beyond

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