BRAHMS-Sensitive Bolometer Arrays for the SPICA Imaging Polarimetry

Rodriguez, L.; Poglitsch, A.; Aliane, A.; Martignac, J.; Dubreuil, Didier; Dussopt, Laurent; Revéret, V.; Goudon, V.; Bounissou, Sophie; Adami, O.-A.; Delisle, Cyrille; Gevin, O.; Broïse, Xavier de la; Maffei, B.; Sauvageot, J. L.

doi:10.1007/s10909-018-2000-6

Cited by 9 publications

(7 citation statements)

References 8 publications

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“…To study the interaction between turbulence, magnetic fields, feedback, and gravity within molecular clouds, we require detailed polarization maps that can both resolve magnetic fields on <<0.1 pc scales of cores and filaments, while also having the sensitivity to produce highfidelity maps of the emission from low-column-density molecular cloud envelopes. Balloonborne polarimeters will soon produce sub-arcmin resolution maps of many molecular clouds; however, higher sensitivity and resolution maps are needed from next-generation satellites such as OST (Staguhn et al, 2018) and SPICA (Rodriguez et al, 2018).…”

Section: Discussionmentioning

confidence: 99%

Studying Magnetic Fields in Star Formation and the Turbulent Interstellar Medium

Fissel,

Hull,

Clark

et al. 2019

Preprint

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Understanding the physics of how stars form is a highly-prioritized goal of modern Astrophysics, in part because star formation is linked to both galactic dynamics on large scales and to the formation of planets on small scales. It is well-known that stars form from the gravitational collapse of molecular clouds, which are in turn formed out of the turbulent interstellar medium. Star formation is highly inefficient, with one of the likely culprits being the regulation against gravitational collapse provided by magnetic fields. Measurement of the polarized emission from interstellar dust grains, which are partially aligned with the magnetic field, provides a key tool for understanding the role these fields play in the star formation process.Over the past decade, much progress has been made by the most recent generation of polarimeters operating over a range of wavelengths (from the far-infrared through the millimeter part of the spectrum) and over a range of angular resolutions (from less than an arcsecond through fractions of a degree). Future developments in instrument sensitivity for ground-based, airborne, and space-borne polarimeters operating over range of spatial scales are critical for enabling revolutionary steps forward in our understanding of the magnetized turbulence from which stars are formed.

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Section: Discussionmentioning

confidence: 99%

Studying Magnetic Fields in Star Formation and the Turbulent Interstellar Medium

Fissel,

Hull,

Clark

et al. 2019

Preprint

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“…It provides wide field 70 − 350 µm polarimetric images in Stokes Q and U of comparable quality (in terms of resolution, signal-to-noise ratio, and both intensity and spatial dynamic ranges) to Herschel images in Stokes I. More details about the B-BOP instrument are in Rodriguez et al (2018) and André et al (2019).…”

Section: B-bopmentioning

confidence: 99%

The role of SPICA-like missions and the Origins Space Telescope in the quest for heavily obscured AGN and synergies with Athena

Barchiesi

Pozzi

Vignali

et al. 2021

Publ. Astron. Soc. Aust.

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In the black hole (BH)–galaxy co-evolution framework, most of the star formation (SF) and the BH accretion are expected to take place in highly obscured conditions. The large amount of gas and dust absorbs most of the UV-to-soft-X radiation and re-emits it at longer wavelengths, mostly in the IR. Thus, obscured active galactic nuclei (AGN) are very difficult to identify in optical or X-ray bands but shine bright in the IR. Moreover, X-ray background (XRB) synthesis models predict that a large fraction of the yet-unresolved XRB is due to the most obscured (Compton thick, CT: N $_{\text{H}}\ge 10^{24} \,\mathrm{cm}^{-2}$ ) of these AGN. In this work, we investigate the synergies between putative IR missions [using SPace Infrared telescope for Cosmology and Astrophysics (SPICA), proposed for European Space Agency (ESA)/M5 but withdrawn in 2020 October, and Origins Space Telescope, OST, as ‘templates’] and the X-ray mission Athena (Advanced Telescope for High ENergy Astrophysics), which should fly in early 2030s, in detecting and characterising AGN, with a particular focus on the most obscured ones. Using an XRB synthesis model, we estimated the number of AGN and the number of those which will be detected in the X-rays by Athena. For each AGN, we associated an optical-to-Far InfraRed (FIR) spectral energy distribution (SED) from observed AGN with both X-ray data and SED decomposition and used these SEDs to check if the AGN will be detected by SPICA-like or OST at IR wavelengths. We expect that, with the deepest Athena and SPICA-like (or OST) surveys, we will be able to photometrically detect in the IR more than 90% of all the AGN (down to $L_{2-10\text{keV}} \sim 10^{42}\,\mathrm{erg\ s}^{-1}$ and up to $z \sim 10$ ) predicted by XRB synthesis modeling, and we will detect at least half of them in the X-rays. The spectroscopic capabilities of the OST can provide ${\approx}51\,000$ and ${\approx}3\,400$ AGN spectra with $R= 300$ at 25–588 $\unicode[Times]{x03BC}$ m in the wide and deep surveys, respectively, the last one up to $z\approx 4$ . Athena will be extremely powerful in detecting and discerning moderate- and high-luminosity AGN, allowing us to properly select AGN even when the mid-IR torus emission is ‘hidden’ by the host galaxy contribution. We will constrain the intrinsic luminosity and the amount of obscuration for $\sim\!20\%$ of all the AGN (and $\sim\!50\%$ of those with $L_{2-10\text{keV}} > 3.2 \times 10^{43}\,\mathrm{erg\ s}^{-1}$ ) using the X-ray spectra provided by Athena WFI. We find that the most obscured and elusive CT-AGN will be exquisitely sampled by SPICA-like mission or OST and that Athena will allow a fine characterisation of the most luminous ones. This will provide a significant step forward in the process of placing stronger constraints on the yet-unresolved XRB and investigating the BH accretion rate evolution up to very high redshift ( $z \ge 4$ ).

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“…It provides widefield 70 − 350 µm polarimetric images in Stokes Q and U of comparable quality (in terms of resolution, signalto-noise ratio, and both intensity and spatial dynamic ranges) to Herschel images in Stokes I. More details about the B-BOP instrument are in Rodriguez et al (2018) and André et al (2019).…”

Section: B-bopmentioning

confidence: 99%

The role of SPICA-like missions and the Origins Space Telescope in the quest for heavily obscured AGN and synergies with Athena

Barchiesi,

Pozzi,

Vignali

et al. 2021

Preprint

View full text Add to dashboard Cite

In the BH-galaxy co-evolution framework, most of the star-formation (SF) and the black hole (BH) accretion is expected to take place in highly obscured conditions. The large amount of gas and dust absorbs most of the UV-to-soft-X radiation and re-emits it at longer wavelengths, mostly in the IR. Thus, obscured Active Galactic Nuclei (AGN) are very difficult to identify in optical or X-ray bands, but shine bright in the IR. Moreover, X-ray background (XRB) synthesis models predict that a large fraction of the yet-unresolved XRB is due to the most obscured (Compton thick, CT: N H ≥ 10 24 cm −2 ) of these AGN. In this work, we investigate the synergies between putative IR missions (using SPICA, proposed for ESA/M5 but withdrawn in October 2020, and Origins Space Telescope, OST, as 'templates') and the X-ray mission Athena, which should fly in early 2030s, in detecting and characterizing AGN, with a particular focus on the most obscured ones. Using an XRB synthesis model, we estimated the number of AGN and the number of those which will be detected in the X-rays by Athena. For each AGN we associated an optical-to-FIR spectral energy distribution (SED) from observed AGN with both X-ray data and SED decomposition, and used these SEDs to check if the AGN will be detected by SPICA-like or OST at IR wavelengths. We expect that, with the deepest Athena and SPICA-like (or OST) surveys, we will be able to photometrically detect in the IR more than 90 % of all the AGN (down to L 2−10keV ∼ 10 42 erg/s and up to z ∼ 10) predicted by XRB synthesis modeling, and we will detect at least half of them in the X-rays. The spectroscopic capabilities of the OST can provide ≈ 51 000 and ≈ 3400 AGN spectra with R= 300 at 25 − 588 µm in the wide and deep surveys, respectively, the last one up to z ≈ 4. Athena will be extremely powerful in detecting and discerning moderate-and high-luminosity AGN, allowing us to properly select AGN even when the mid-IR torus emission is "hidden" by the host-galaxy contribution. We will constrain the intrinsic luminosity and the amount of obscuration for ∼ 20 % of all the AGN (and ∼ 50 % of those with L 2−10keV > 3.2 × 10 43 erg/s) using the X-ray spectra provided by Athena WFI. We find that the most obscured and elusive CT-AGN will be exquisitely sampled by SPICA-like mission or OST and that Athena will allow a fine characterization of the most-luminous ones. This will provide a significant step forward in the process of placing stronger constraints on the yet-unresolved XRB and investigating the BH accretion rate evolution up to very high redshift (z ≥ 4).

show abstract

BRAHMS-Sensitive Bolometer Arrays for the SPICA Imaging Polarimetry

Cited by 9 publications

References 8 publications

Studying Magnetic Fields in Star Formation and the Turbulent Interstellar Medium

Studying Magnetic Fields in Star Formation and the Turbulent Interstellar Medium

The role of SPICA-like missions and the Origins Space Telescope in the quest for heavily obscured AGN and synergies with Athena

The role of SPICA-like missions and the Origins Space Telescope in the quest for heavily obscured AGN and synergies with Athena

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