Metallicity diagnostics with infrared fine-structure lines

Nagao, Tohru; Maiolino, R.; Marconi, A.; Matsuhara, Hideo

doi:10.1051/0004-6361/201015471

Cited by 93 publications

(124 citation statements)

References 66 publications

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“…These fiducial values for nH and U are close to the parameters used in Fig. 2 of Nagao et al (2011), where HII regions represent MC outskirts with column density 4 × 10 20 cm −2 . From this figure, we can see that in correspondence of the MC column density expected by the V15 model (∼ 3 × 10 21 cm −2 ) the [C II] emission is almost 50 time stronger than the one at the edge of the HII regions, implying that the latter only contribute fHII ∼ 2% to the total emission.…”

Section: Conclusion and Discussionsupporting

confidence: 77%

Intensity mapping of [C ii] emission from early galaxies

Yue

Ferrara

Pallottini

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The intensity mapping of the [C II] 157.7 µm fine-structure emission line represents an ideal experiment to probe star formation activity in galaxies, especially in those that are too faint to be individually detected. Here, we investigate the feasibility of such an experiment for z > 5 galaxies. We construct the L CII − M h relation from observations and simulations, then generate mock [C II] intensity maps by applying this relation to halo catalogs built from large scale N-body simulations. Maps of the extragalactic farinfrared (FIR) continuum, referred to as "foreground", and CO rotational transition lines and [C I] fine-structure lines referred to as "contamination", are produced as well. We find that, at 316 GHz (corresponding to z CII = 5), the mean intensities of the extragalactic FIR continuum, [C II] signal, all CO lines from J = 1 to 13 and two [C I] lines are ∼ 3 × 10 5 Jy sr −1 , ∼ 1200 Jy sr −1 , ∼ 800 Jy sr −1 and ∼ 100 Jy sr −1 , respectively. We discuss a method that allows us to subtract the FIR continuum foreground by removing a spectrally smooth component from each line of sight, and to suppress the CO/[C I] contamination by discarding pixels that are bright in contamination emission. The z > 5 [C II] signal comes mainly from halos in the mass range 10 11−12 M ⊙ ; as this mass range is narrow, intensity mapping is an ideal experiment to investigate these early galaxies. In principle such signal is accessible to a ground-based telescope with a 6 m aperture, 150 K system temperature, a 128 × 128 pixels FIR camera in 5000 hr total integration time, however it is difficult to perform such an experiment by using currently available telescopes.

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Section: Conclusion and Discussionsupporting

confidence: 77%

Intensity mapping of [C ii] emission from early galaxies

Yue

Ferrara

Pallottini

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…∼ 0.07 Z ) on our results but find little difference for the main quantities of interest. We adopt all gas element abundances for solar metallicity from Nagao et al (2011) and include Orion-like dust and magnetic fields (intensity of 10 −5 G at the inner edge, as appropriate for the Orion nebula according to the Cloudy documentation). We fix the cloud inner edge gas density and ionization parameter (U) for starburst ages of 1 Myr and 10 Myr, and vary both parameters in a grid.…”

Section: Cloudy Modeling Of the [Cii]/[nii] Ratiomentioning

confidence: 99%

ALMA REVEALS WEAK [N ii] EMISSION IN “TYPICAL” GALAXIES AND INTENSE STARBURSTS AT z = 5–6

Pavesi

Riechers

Capak

et al. 2016

ApJ

132

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We report interferometric measurements of [Nii] 205 µm fine-structure line emission from a representative sample of three galaxies at z = 5-6 using the Atacama Large (sub)Millimeter Array (ALMA). These galaxies were previously detected in [Cii] and far-infrared continuum emission and span almost two orders of magnitude in star formation rate (SFR). Our results show at least two different regimes of ionized inter-stellar medium properties for galaxies in the first billion years of cosmic time, separated by theirUV star-forming galaxy, likely directly or indirectly (by its effect on the radiation field) related to low dust abundance and low metallicity. The infrared-luminous modestly star-forming Lyman Break Galaxy (LBG) in our sample is characterized by an ionized-gas fraction (L [CII] /L [NII] 20) typical of local star-forming galaxies and shows evidence for spatial variations in its ionized-gas fraction across an extended gas reservoir. The extreme SFR, warm and compact dusty starburst AzTEC-3 shows an ionized fraction higher than expected given its star-formation rate surface densitydominantly traces a diffuse ionized medium rather than star-forming Hii regions in this type of galaxy. This highest redshift sample of [Nii] detections provides some of the first constraints on ionized and neutral gas modeling attempts and on the structure of the inter-stellar medium at z = 5-6 in "normal" galaxies and starbursts.

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“…With a critical density ∼10 5 cm −3 for collisions with neutral hydrogen and ∼10 2 cm −3 for collisions with electrons, and a low ionization potential of 8.15 eV, this line comes from a wide variety of regions, such as ionized gas and warm atomic gas, PDRs, and X-ray-dominated regions (XDRs; Hollenbach & Tielens 1999). H ii regions represent a large fraction of [Si ii]34.8 μm emission in the ring (between 30% and 60%; e.g., Nagao et al 2011). We used an [Si ii]34.8 μm image of the ring and Enuc S, and convolved it to the 160 μm Herschel-PACS beam using theoretical Spitzer-IRS PSFs made with STinyTim and Herschel PSFs calculated by Aniano et al (2011).…”

Section: However They Find a Large Scatter In ([C Ii]+[o I])/f (5-10mentioning

confidence: 99%

A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITHHERSCHEL-PACS ANDSPITZER-IRS

Beirão

Armus

Hélou

et al. 2012

ApJ

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NGC 1097 is a nearby Seyfert 1 galaxy with a bright circumnuclear starburst ring, a strong large-scale bar, and an active nucleus. We present a detailed study of the spatial variation of the far-infrared (FIR) [C ii]158 μm and [O i]63 μm lines and mid-infrared H 2 emission lines as tracers of gas cooling, and of the polycyclic aromatic hydrocarbon (PAH) bands as tracers of the photoelectric heating, using Herschel-PACS and Spitzer-IRS infrared spectral maps. We focus on the nucleus and the ring, and two star-forming regions (Enuc N and Enuc S). We estimated a photoelectric gas heating efficiency ([C ii]158 μm+[O i]63 μm)/PAH in the ring about 50% lower than in Enuc N and S. The average 11.3/7.7 μm PAH ratio is also lower in the ring, which may suggest a larger fraction of ionized PAHs, but no clear correlation with [C ii]158 μm/PAH(5.5-14 μm) is found. PAHs in the ring are responsible for a factor of two more [C ii]158 μm and [O i]63 μm emission per unit mass than PAHs in the Enuc S. spectral energy distribution (SED) modeling indicates that at most 25% of the FIR power in the ring and Enuc S can come from high-intensity photodissociation regions (PDRs), in which case G 0 ∼ 10 2.3 and n H ∼ 10 3.5 cm −3 in the ring. For these values of G 0 and n H , PDR models cannot reproduce the observed H 2 emission. Much of the H 2 emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks.

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Metallicity diagnostics with infrared fine-structure lines

Cited by 93 publications

References 66 publications

Intensity mapping of [C ii] emission from early galaxies

Intensity mapping of [C ii] emission from early galaxies

ALMA REVEALS WEAK [N ii] EMISSION IN “TYPICAL” GALAXIES AND INTENSE STARBURSTS AT z = 5–6

A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITHHERSCHEL-PACS ANDSPITZER-IRS

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