The Mid‐Infrared Spectrum of Star‐forming Galaxies: Global Properties of Polycyclic Aromatic Hydrocarbon Emission

Smith, John David; Draine, B. T.; Dale, Daniel A.; Moustakas, John; Kennicutt, Robert C.; Hélou, G.; Armus, L.; Roussel, H.; Sheth, Kartik; Bendo, G. J.; Buckalew, B.; Calzetti, Daniela; Engelbracht, C. W.; Gordon, K. D.; Hollenbach, D. J.; Li, A.; Malhotra, Sangeeta; Murphy, E. J.; Walter, Fabian

doi:10.1086/510549

Cited by 878 publications

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References 90 publications

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“…Smith et al 2007;Draine & Li 2007;Vogler et al 2005;Lu et al 2003;Genzel & Cesarksky 2000, and references therein) and, as indicated in Sect. 1, the λ 6.75 µm ISO band is no exception.…”

Section: The λ 675 µM Emissionmentioning

confidence: 82%

“…7 of Irwin & Madden 2006) and can be modeled as a blend of three spectral features at λ 7.42 µm, λ 7.60 µm, and λ 7.85 µm (Smith et al 2007). The λ 7.7 µm PAH complex, alone, can contribute nearly one-half of the total PAH luminosity and up to 10% of the total infrared luminosity (Smith et al 2007). Indeed, photometry of the λ 6.75 µm ISO band is normally taken as a direct proxy for the presence of PAH emission.…”

Section: The λ 675 µM Emissionmentioning

confidence: 99%

“…The ratios between the λ 6.2, λ 7.7, and λ 8.6 µm PAHs do not seem to show much variation within galaxies and between galaxies (Galliano et al 2007), but the λ 6.2/λ 11.3 and λ 7.7/λ 11.3 ratios can vary by up to an order of magnitude (Lu et al 2003;Vogler et al 2005;Draine & Li 2007;Smith et al 2007;Galliano et al 2007). This variation can be controlled by the fraction of ionized PAHs, which has been demonstrated to be linked to G 0 /n e (the ratio of the intensity of the UV radiation field to the electron density, Galliano et al 2007) or to the modification of the grain size distribution (Smith et al 2007). For this study, since we are dealing only with the λ 6.75 µm ISOCAM band, we can assume constant band ratios between the λ 6.2, λ 7.7 and λ 8.6 µm PAH features, although some variation will not affect our conclusions.…”

Section: The λ 675 µM Emissionmentioning

confidence: 99%

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PAHs in the halo of NGC 5529

Irwin¹,

Kennedy²,

Parkin³

et al. 2007

A&A

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We present sensitive ISO λ 6.7 µm observations of the edge-on galaxy, NGC 5529, finding an extensive MIR halo around NGC 5529. The emission is dominated by PAHs in this band. The PAH halo has an exponential scale height of 3.7 kpc but can still be detected as far as ≈10 kpc from the plane to the limits of the high dynamic range (1770/1) data. This is the most extensive PAH halo yet detected in a normal galaxy. This halo shows substructure and the PAHs likely originate from some type of disk outflow. PAHs are long-lived in a halo environment and therefore continuous replenishment from the disk is not required (unless halo PAHs are also being destroyed or removed), consistent with the current low SFR of the galaxy. The PAHs correlate spatially with halo Hα emission, previously observed by Miller & Veilleux (2003, ApJS, 148, 383); both components are likely excited/ionized by in-disk photons that are leaking into the halo. The presence of halo gas may be related to the environment of NGC 5529 which contains at least 17 galaxies in a small group of which NGC 5529 is the dominant member. Of these, we have identified two new companions from the SDSS.Key words. galaxies: general -galaxies: individual: NGC 5529 -galaxies: halos -galaxies: ISM IntroductionNearby edge-on galaxies provide an important local laboratory for understanding physical conditions in the disk-halo interface. This critical region separates two very different environments over a relatively small vertical distance. It plays an important role in a galaxy's energy balance as well as its chemical evolution, since outflows from the disk, circulating "fountains", and possibly infalling external material may each be involved at some point in a galaxy's evolution. Moreover, knowledge of the physical conditions of outflowing gas in nearby galaxies can provide important constraints on galaxy formation scenarios, since outflows (i.e. some form of "feedback") are crucial to these models (e.g. Marri & White 2003, and others). Nearby edgeon galaxies have now been studied in many wavebands showing a variety of interstellar medium (ISM) components above the galactic disk. Indeed, in at least one galaxy that has a high star formation rate (SFR), every component of the interstellar medium, including dust, molecular gas, HI, extra-planar diffuse ionized gas (eDIG, detected by Hα emission) and X-ray emitting hot gas has been detected above the galactic disk (see Lee et al. 2001;and Brar et al. 2003). In each component, discrete disk-halo vertical structures are seen, suggestive of outflow.The recent discovery, from mid-infrared (MIR) observations, of PAH (polycyclic aromatic hydrocarbon) emission 1 in the halo of the low SFR galaxy, NGC 5907 (Irwin & Madden 2006), has prompted a search for other galaxies that may show similar emission. In this paper, we present results for the edge-on galaxy, NGC 5529, using archival data from the Infrared Space 1 There is some uncertainty as to the nature of the carriers of the MIR band emission. In this paper, we adopt the PAH...

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“…Smith et al 2007;Draine & Li 2007;Vogler et al 2005;Lu et al 2003;Genzel & Cesarksky 2000, and references therein) and, as indicated in Sect. 1, the λ 6.75 µm ISO band is no exception.…”

Section: The λ 675 µM Emissionmentioning

confidence: 82%

Section: The λ 675 µM Emissionmentioning

confidence: 99%

Section: The λ 675 µM Emissionmentioning

confidence: 99%

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PAHs in the halo of NGC 5529

Irwin¹,

Kennedy²,

Parkin³

et al. 2007

A&A

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“…(9) 60 (38) 157 (101) 310 (193) 185 (104) 310 (110) 12.50−13.00 37 (28) 276 (231) 710 (576) 1240 (934) 1639 (1054) 596 (195) 146 (5) 12. 25−12.50 130 (114) 701 (631) 1264 (1068) 1270 (852) 694 (45) 84 (0) (6217) 4365 (3178) 3248 (1921) 2732 (1293) 864 (299) 456 (116) used PAHFIT (Smith et al 2007), assuming a powerlaw continuum and an extinction curve with a screen configuration (Kemper et al 2004). Free parameters are the normalizations of the PAH features, the normalization and the index of the power-law continuum, and the extinction.…”

Section: Characterization Of Pahsmentioning

confidence: 99%

Unbiased Large Spectroscopic Surveys of Galaxies Selected by SPICA Using Dust Bands

Kaneda

Ishihara

Oyabu

et al. 2017

Publ. Astron. Soc. Aust.

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The mid-infrared (IR) range contains many spectral features associated with large molecules and dust grains such as polycyclic aromatic hydrocarbons (PAHs) and silicates. These are usually very strong compared to fine-structure gas lines, and thus valuable in studying the spectral properties of faint distant galaxies. In this paper, we evaluate the capability of low-resolution mid-IR spectroscopic surveys of galaxies that could be performed by SPICA. The surveys are designed to address the question how star formation and black hole accretion activities evolved over cosmic time through spectral diagnostics of the physical conditions of the interstellar/circumnuclear media in galaxies. On the basis of results obtained with Herschel far-IR photometric surveys of distant galaxies and Spitzer and AKARI near-to mid-IR spectroscopic observations of nearby galaxies, we estimate the numbers of the galaxies at redshift z > 0.5, which are expected to be detected in the PAH features or dust continuum by a wide (10 deg 2 ) or deep (1 deg 2 ) blind survey, both for a given observation time of 600 hours. As by-products of the wide blind survey, we also expect to detect debris disks, through the mid-IR excess above the photospheric emission of nearby main-sequence stars, and we estimate their number. We demonstrate that the SPICA mid-IR surveys will efficiently provide us with unprecedentedly large spectral samples, which can be studied further in the far-IR with SPICA.Keywords: galaxies: evolution -galaxies: star-formation -galaxies: active -infrared: galaxies -infrared: ISM -methods: observational 1 2 Kaneda et al. PrefaceThe following set of papers describe in detail the science goals of the future Space Infrared telescope for Cosmology and Astrophysics (SPICA). The SPICA satellite will employ a 2.5-m telescope, actively cooled to around 6 K, and a suite of mid-to far-IR spectrometers and photometric cameras, equipped with state of the art detectors. In particular the SPICA Far Infrared Instrument (SAFARI) will be a grating spectrograph with low (R = 300) and medium (R ≃ 3000-11000) resolution observing modes instantaneously covering the 35-230 µm wavelength range. The SPICA Mid-Infrared Instrument (SMI) will have three operating modes: a large field of view (12 ′ × 10 ′ ) low-resolution 17-36 µm spectroscopic (R ∼ 50-120) and photometric camera at 34 µm, a medium resolution (R ≃ 2000) grating spectrometer covering wavelengths of 18-36 µm and a highresolution echelle module (R ≃ 28000) for the 12-18 µm domain. A large field of view (80 ′′ × 80 ′′ ), three channel, (110 µm, 220 µm and 350 µm) polarimetric camera will also be part of the instrument complement. These articles will focus on some of the major scientific questions that the SPICA mission aims to address, more details about the mission and instruments can be found in Roelfsema et al. (2017).

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“…Least squares fit of the PAH spectra in the Ames' database to the ISO SWS spectrum of the H ii Region IRAS 23133. From Cami et al (2008) routinely called the "PAH bands" and are used as probes of the ISM in extra-galactic environments (Smith et al 2007). PAHs are also thought to contribute to the interstellar extinction and to be among the carriers of the diffuse interstellar absorption bands (DIBs).…”

Section: Overviewmentioning

confidence: 99%

PAHs in Astronomy - A Review

Salama

2008

Proc. IAU

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Abstract. Carbonaceous materials play an important role in space. Polycyclic Aromatic Hydrocarbons (PAHs) are a ubiquitous component of organic matter in space. Their contribution is invoked in a broad spectrum of astronomical observations that range from the ultraviolet to the far-infrared and cover a wide variety of objects and environments from meteorites and interplanetary dust particles to outer Solar System bodies to the interstellar medium in the local Milky Way and in other galaxies. Extensive efforts have been devoted in the past two decades to experimental, theoretical, and observational studies of PAHs. A brief review is given here of the evidence obtained so far for the contribution of PAHs to the phenomena aforementioned. An attempt is made to distinguish the cases where solid evidence is available from cases where reasonable assumptions can be made to the cases where the presence -or the absence -of PAHs is purely speculative at this point.

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The Mid‐Infrared Spectrum of Star‐forming Galaxies: Global Properties of Polycyclic Aromatic Hydrocarbon Emission

Cited by 878 publications

References 90 publications

PAHs in the halo of NGC 5529

PAHs in the halo of NGC 5529

Unbiased Large Spectroscopic Surveys of Galaxies Selected by SPICA Using Dust Bands

PAHs in Astronomy - A Review

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