The X-ray emission of local luminous infrared galaxies

We present new mid-infrared N -band spectroscopy and Q-band photometry of the local luminous infrared galaxy NGC 1614, one of the most extreme nearby starbursts. We analyze the mid-IR properties of the nucleus (central 150 pc) and four regions of the bright circumnuclear (diameter∼ 600 pc) star-forming (SF) ring of this object. The nucleus differs from the circumnuclear SF ring by having a strong 8-12 µm continuum (low 11.3 µm PAH equivalent width). These characteristics, together with the nuclear X-ray and sub-mm properties, can be explained by an X-ray weak active galactic nucleus (AGN), or by peculiar SF with a short molecular gas depletion time and producing an enhanced radiation field density. In either case, the nuclear luminosity (L IR <6×10 43 erg s −1 ) is only <5 % of the total bolometric luminosity of NGC 1614. So this possible AGN does not dominate the energy output in this object. We also compare three star-formation rate (SFR) tracers (Paα, 11.3 µm PAH, and 24 µm emissions) at 150 pc scales in the circumnuclear ring. In general, we find that the SFR is underestimated (overestimated) by a factor of 2-4 (2-3) using the 11.3 µm PAH (24 µm) emission with respect to the extinction corrected Paα SFR. The former can be explained because we do not include diffuse PAH emission in our measurements, while the latter might indicate that the dust temperature is particularly warmer in the central regions of NGC 1614.

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“…Similarly, the soft X-ray emission is also better explained by star-formation (Pereira-Santaella et al 2011;Herrero-Illana et al 2014).…”

Section: Weak X-ray Emissionmentioning

confidence: 93%

Sub-arcsec mid-IR observations of NGC 1614: Nuclear star formation or an intrinsically X-ray weak AGN?

Pereira-Santaella¹,

Colina²,

Alonso‐Herrero³

et al. 2015

Mon. Not. R. Astron. Soc.

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“…16). For the local Universe we compared our results with samples presented by U et al (2012), Symeonidis et al (2013), Pereira-Santaella et al (2011), andClements et al (2010) (Fig. 16, left panel).…”

Section: Luminosity/temperature Relationmentioning

confidence: 99%

[Ultra] luminous infrared galaxies selected at 90μm in the AKARI deep field: a study of AGN types contributing to their infrared emission

Małek

Bankowicz

Pollo

et al. 2017

A&A

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Aims. The aim of this work is to characterize physical properties of ultra luminous infrared galaxies (ULIRGs) and luminous infrared galaxies (LIRGs) detected in the far-infrared (FIR) 90 µm band in the AKARI Deep Field-South (ADF-S) survey. In particular, we want to estimate the active galactic nucleus (AGN) contribution to the LIRGs and ULIRGs' infrared emission and which types of AGNs are related to their activity. Methods. We examined 69 galaxies at redshift ≥0.05 detected at 90 µm by the AKARI satellite in the ADF-S, with optical counterparts and spectral coverage from the ultraviolet to the FIR. We used two independent spectral energy distribution fitting codes: one fitting the SED from FIR to FUV (CIGALE) (we use the results from CIGALE as a reference) and gray-body + power spectrum fit for the infrared part of the spectra (CMCIRSED) in order to identify a subsample of ULIRGs and LIRGs, and to estimate their properties. Results. Based on the CIGALE SED fitting, we have found that LIRGs and ULIRGs selected at the 90 µm AKARI band compose ∼56% of our sample (we found 17 ULIRGs and 22 LIRGs, spanning over the redshift range 0.06 < z < 1.23). Their physical parameters, such as stellar mass, star formation rate (SFR), and specific SFR are consistent with the ones found for other samples selected at infrared wavelengths. We have detected a significant AGN contribution to the mid-infrared luminosity for 63% of LIRGs and ULIRGs. Our LIRGs contain Type 1, Type 2, and intermediate types of AGN, whereas for ULIRGs, a majority (more than 50%) of AGN emission originates from Type 2 AGNs. The temperature-luminosity and temperature-mass relations for the dust component of ADF-S LIRGs and ULIRGs indicate that these relations are shaped by the dust mass and not by the increased dust heating. Conclusions. We conclude that LIRGs contain Type 1, Type 2, and intermediate types of AGNs, with an AGN contribution to the mid infrared emission at the median level of 13 ± 3%, whereas the majority of ULIRGs contain Type 2 AGNs, with a median AGN fraction equal to 19 ± 8%.

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“…This X-ray emission produced due to X-ray binaries (L X,SF ) is an obvious source of contamination in our total X-ray stacked luminosity (L X,tot ). We estimate and statistically remove L X,SF from L X,tot by calculating the logmean SFR and M * of the stacked galaxy sample and invoking the local relations of Lehmer et al (2010) and Pereira-Santaella et al (2011). Specifically, in the 0.5-2keV band, we use Equation (4) presented in Pereira-Santaella et al (2011), and in the 2-7keV band, we use the SFR-dependent relation logL 39.46 0.76 X = + logSFR presented in Lehmer et al (2010), and linearly combine both L X,SF predictions in the 0.5-7keV.…”

Section: The Average Accretion Rate Of (Un)-barred Spiral Galaxiesmentioning

confidence: 99%

Galaxy-scale Bars in Late-type Sloan Digital Sky Survey Galaxies Do Not Influence the Average Accretion Rates of Supermassive Black Holes

Goulding

Matthaey

Greene

et al. 2017

ApJ

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Galaxy-scale bars are expected to provide an effective means for driving material towards the central region in spiral galaxies, and possibly feeding supermassive black holes (BHs). Here we present a statistically-complete study of the effect of bars on average BH accretion. From a well-selected sample of 50,794 spiral galaxies (with M * ∼ 0.2 − 30 × 10 10 M ) extracted from the Sloan Digital Sky Survey Galaxy Zoo 2 project, we separate those sources considered to contain galaxy-scale bars from those that do not. Using archival data taken by the Chandra X-ray Observatory, we identify X-ray luminous (L X 10 41 erg s −1 ) active galactic nuclei (AGN) and perform an X-ray stacking analysis on the remaining X-ray undetected sources. Through X-ray stacking, we derive a time-averaged look at accretion for galaxies at fixed stellar mass and star formation rate, finding that the average nuclear accretion rates of galaxies with bar structures are fully consistent with those lacking bars ( Ṁacc ≈ 3 × 10 −5 M yr −1 ). Hence, we robustly conclude that large-scale bars have little or no effect on the average growth of BHs in nearby (z < 0.15) galaxies over gigayear timescales.

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The X-ray emission of local luminous infrared galaxies

Cited by 94 publications

References 113 publications

Sub-arcsec mid-IR observations of NGC 1614: Nuclear star formation or an intrinsically X-ray weak AGN?

Sub-arcsec mid-IR observations of NGC 1614: Nuclear star formation or an intrinsically X-ray weak AGN?

[Ultra] luminous infrared galaxies selected at 90μm in the AKARI deep field: a study of AGN types contributing to their infrared emission

Galaxy-scale Bars in Late-type Sloan Digital Sky Survey Galaxies Do Not Influence the Average Accretion Rates of Supermassive Black Holes

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