The space infrared telescope for cosmology and astrophysics: SPICA A joint mission between JAXA and ESA

Swinyard, Bruce; Nakagawa, Takao

doi:10.1007/s10686-008-9090-0

Cited by 111 publications

(86 citation statements)

References 26 publications

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“…Although the line shown in Fig. 8 cannot be observed with currently available instruments, future missions such as SPICA are expected to have a higher resolution and sensitivity than Herschel to measure the O I and C II lines (Swinyard et al 2009) from which our model can be used to make predictions. Assuming this scenario, one should add the oxygen coming from water to the original oxygen number density coming from CO.…”

Section: How To Also Fit the Apex C I Non-detection?mentioning

confidence: 99%

A self-consistent model for the evolution of the gas produced in the debris disc of β Pictoris

Kral¹,

Wyatt²,

Carswell³

et al. 2016

Mon. Not. R. Astron. Soc.

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This paper presents a self-consistent model for the evolution of gas produced in the debris disc of β Pictoris. Our model proposes that atomic carbon and oxygen are created from the photodissociation of CO, which is itself released from volatile-rich bodies in the debris disc due to grain-grain collisions or photodesorption. While the CO lasts less than one orbit, the atomic gas evolves by viscous spreading resulting in an accretion disc inside the parent belt and a decretion disc outside. The temperature, ionisation fraction and population levels of carbon and oxygen are followed with the photodissociation region model Cloudy, which is coupled to a dynamical viscous α model. We present new gas observations of β Pic, of C I observed with APEX and O I observed with Herschel, and show that these along with published C II and CO observations can all be explained with this new model. Our model requires a viscosity α > 0.1, similar to that found in sufficiently ionised discs of other astronomical objects; we propose that the magnetorotational instability is at play in this highly ionised and dilute medium. This new model can be tested from its predictions for high resolution ALMA observations of C I. We also constrain the water content of the planetesimals in β Pic. The scenario proposed here might be at play in all debris discs and this model could be used more generally on all discs with C, O or CO detections.

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Section: How To Also Fit the Apex C I Non-detection?mentioning

confidence: 99%

A self-consistent model for the evolution of the gas produced in the debris disc of β Pictoris

Kral¹,

Wyatt²,

Carswell³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…In our first example, we envision an instrument on the planned Space Infrared Telescope for Cosmology and Astrophysics (SPICA) [27]. SPICA is a 3.5 meter space-borne infrared telescope planned for launch in 2017.…”

Section: Spica a Instrumentmentioning

confidence: 99%

Demonstrating the feasibility of line intensity mapping using mock data of galaxy clustering from simulations

Visbal

Trac

Loeb

2011

J. Cosmol. Astropart. Phys.

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Visbal & Loeb (2010) have shown that it is possible to measure the clustering of galaxies by cross correlating the cumulative emission from two different spectral lines which originate at the same redshift. Through this cross correlation, one can study galaxies which are too faint to be individually resolved. This technique, known as intensity mapping, is a promising probe of the global properties of high redshift galaxies. Here, we test the feasibility of such measurements with synthetic data generated from cosmological dark matter simulations. We use a simple prescription for associating galaxies with dark matter halos and create a realization of emitted radiation as a function of angular position and wavelength over a patch of the sky. This is then used to create synthetic data for two different hypothetical instruments, one aboard the Space Infrared Telescope for Cosmology and Astrophysics (SPICA) and another consisting of a pair of ground based radio telescopes designed to measure the CO(1-0) and CO(2-1) emission lines. We find that the line cross power spectrum can be measured accurately from the synthetic data with errors consistent with the analytical prediction of Visbal & Loeb (2010). Removal of astronomical backgrounds and masking bright line emission from foreground contaminating galaxies do not prevent accurate cross power spectrum measurements.

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“…2 The promise of SPICA With its expected exceptional sensitivity and spectroscopic capabilities (Swinyard et al 2009;Nakagawa et al 2014;Sibthorpe et al 2016;Spinoglio et al 2017), the far-IR observatory SPICA would address these questions by spectroscopically observing galaxies from z = 0 to z ∼ 1.5 in multiple molecular and atomic lines. The SpicA FAR Infrared instrument (SAFARI) (Swinyard et al 2009;Pastor et al 2016;Spinoglio et al 2017), covering the wavelength range 34 − 230 µm, is designed to provide two spectroscopic observing modes, the low-resolution (LR) mode with nominal R nom = 300, and the high-resolution (HR) Feedback and feeding with SPICA 5 Figure 2.…”

Section: Introductionmentioning

confidence: 99%

“…The SpicA FAR Infrared instrument (SAFARI) (Swinyard et al 2009;Pastor et al 2016;Spinoglio et al 2017), covering the wavelength range 34 − 230 µm, is designed to provide two spectroscopic observing modes, the low-resolution (LR) mode with nominal R nom = 300, and the high-resolution (HR) Feedback and feeding with SPICA 5 Figure 2. The equivalent width of the OH65 doublet at systemic velocities (−200 to +200 km s −1 ), probing buried and warm sources in the far-IR, as a function of V 84 (OH119) -84% of the absorption in the OH119 doublet is produced at velocities more positive than V 84 , so that this quantity is a measure of the outflow velocity (Veilleux et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Feedback and Feeding in the Context of Galaxy Evolution withSPICA: Direct Characterisation of Molecular Outflows and Inflows

González-Alfonso

Armus

Carrera

et al. 2017

Publ. Astron. Soc. Aust.

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A far-infrared observatory such as the SPace Infrared telescope for Cosmology and Astrophysics (SPICA), with its unprecedented spectroscopic sensitivity, would unveil the role of feedback in galaxy evolution during the last ∼ 10 Gyr of the Universe (z = 1.5 − 2), through the use of far-and mid-infrared molecular and ionic fine structure lines that trace outflowing and infalling gas. Outflowing gas is identified in the far-infrared through P-Cygni line shapes and absorption blueshifted wings in molecular lines with high dipolar moments, and through emission line wings of fine-structure lines of ionized gas. We quantify the detectability of galaxy-scale massive molecular and ionized outflows as a function of redshift in AGN-dominated, starburstdominated, and main-sequence galaxies, explore the detectability of metal-rich inflows in the local Universe, and describe the most significant synergies with other current and future observatories that will measure feedback in galaxies via complementary tracers at other wavelengths.

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The space infrared telescope for cosmology and astrophysics: SPICA A joint mission between JAXA and ESA

Cited by 111 publications

References 26 publications

A self-consistent model for the evolution of the gas produced in the debris disc of β Pictoris

A self-consistent model for the evolution of the gas produced in the debris disc of β Pictoris

Demonstrating the feasibility of line intensity mapping using mock data of galaxy clustering from simulations

Feedback and Feeding in the Context of Galaxy Evolution withSPICA: Direct Characterisation of Molecular Outflows and Inflows

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