Feedback and Feeding in the Context of Galaxy Evolution with<i>SPICA</i>: Direct Characterisation of Molecular Outflows and Inflows

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.

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

“…George (2015), for all three lines; Brisbin et al(2015)and Farrah et al (2013), for the [O I] 63.18 and [C II] 157.7 µm lines; and Oteo et al (2016), Gullberg et al (2015), Schaerer et al (2015), Yun et al (2015), and Magdis et al…”

mentioning

confidence: 96%

Origins Space Telescope: Predictions for far-IR spectroscopic surveys

Bonato

Zotti

Leisawitz

et al. 2019

“…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.…”

Section: The Power Of Infrared Diagnosticsmentioning

confidence: 99%

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

Roelfsema

Shibai

Armus

et al. 2018

Self Cite

101

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.

“…For example, a 2 000-h SAFARI survey will obtain low-resolution (LR; R = 300) spectra for over 1 000 galaxies up to z 4 (Spinoglio et al 2017) while a 600-h SMI survey will identify about 50 000 galaxies in a 10 deg 2 area through R = 50-120 spectroscopy of polycyclic aromatic hydrocarbon (PAH) emission features (Kaneda et al 2017). Such data sets will enormously advance our understanding of galaxy/AGN evolution and will shed light on key science topics such as chemical evolution/metal enrichment (Fernández-Ontiveros et al 2017) and molecular outflows/inflows (González-Alfonso et al 2017). Note that the great power of SPICA mainly resides in such spectroscopic observations, especially in the far-infrared (>100 μm), where Herschel/Spectral and Photometric Imaging Receiver (SPIRE) has already achieved confusion-limited broad-band imaging sensitivities with a 3.5-m telescope.…”

Section: Introductionmentioning

confidence: 99%

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

Egami

Gallerani

Schneider

et al. 2018

Self Cite

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.