Sasmirala Individual Information for NGC 5506

Description

NGC 5506 is a peculiar edge-on spiral galaxy at a redshift of z = 0.0062 (D ~ 31.6 Mpc) with an AGN classified as a Sy 1.9, a narrow-line Sy 1 or a Sy 2 nucleus (see discussion in [trippe_multi-wavelength_2010]). Broad emission lines are detected in the near-infrared [nagar_ngc_2002]. NGC 5506 is very bright in X-rays and is included in the nine-month BAT AGN sample. At radio wavelengths, it features a compact nucleus embedded within a halo elongated towards the North with ~ 3arcsec ~ 450 pc extent [wehrle_unusual_1987]. On milliarcsecond-scales, the nucleus is further resolved into a double source along a PA~ 70^∘ [kinney_jet_2000]. In addition, a nuclear water maser was detected [braatz_discovery_1994]. The [O III] emission extends over several kiloparsecs and is elongated in the north-south direction [wilson_kinematics_1985]. The first ground-based MIR observations of NGC 5506 were performed by [roche_8-13_1984] in 1981 and 1982, followed by [ward_continuum_1987], [telesco_genesis_1993], and [maiolino_new_1995]. Additional low-angular resolution spectrophotometry was obtained with ISO [rigopoulou_large_1999, tran_isocam-cvf_2001]. The first subarcsecond N-band images were obtained with Palomar 5 m/MIRLIN in 2000 [gorjian_10_2004], followed by N-band spectrophotometry with ESO 3.6 m/TIMMI2 in 2001 and 2002 [siebenmorgen_isocam_2004, raban_core_2008]. An unresolved nucleus was detected in all these images, but the 11.9 μm image from [raban_core_2008] indicates extended emission towards the north-east. The Spitzer/IRAC and MIPS images are dominated by a bright compact nucleus with extended host emission visible in the IRAC images. The nucleus is saturated in the PBCD IRAC images and, thus, not analysed here (but see [gallimore_infrared_2010]). The Spitzer/IRS LR staring-mode spectrum exhibits deep silicate 10 μm and weak silicate 18 μm absorption, very weak PAH emission and a flat spectral slope in νF_ν-space (see also [shi_9.7_2006, wu_spitzer/irs_2009, tommasin_spitzer-irs_2010, gallimore_infrared_2010, mullaney_defining_2011]). Therefore, contribution of star formation to the arcsecond-scale MIR SED is probably minor. The SED flux levels agree with the historical data within the uncertainties, which are dominated by the steep N-band slopes caused by the silicate absorption. The nuclear region of NGC 5506 was observed with T-ReCS in N-band imaging and spectroscopic modes in 2004 [roche_silicate_2007], with Michelle in the N’ and Qa filters [ramos_almeida_infrared_2009], and with VISIR in four N and one Q band filters in 2005, 2006 and 2010 (partly published in [haas_visir_2007, reunanen_vlt_2010]). In all cases, a compact nucleus without further host emission was detected. The nucleus appears marginally resolved but is not intrinsically elongated in the sharpest images (FWHM~ 0.4arcsec ~ 60 pc). The only exception might be the Si6 image, for which no matching standard star observation could be found. Therefore, we treat the Si6 measurement as an upper limit for the unresolved nuclear emission. In neither of the images did we clearly detect the extended emission seen in the TIMMI2 11.9 μm, although some images may hint towards a slight extension in eastern direction. Our nuclear photometry is generally consistent with [ramos_almeida_infrared_2009] and [reunanen_vlt_2010], and on average ~ 26% lower than the Spitzer spectrophotometry. Note that the Michelle measurements are significantly higher than the other subarcsecond measurements because they were obtained in substandard seeing conditions. The nuclear MIR SED indicates the same silicate 10 μm absorption feature as seen in the arcsecond-scale MIR SED. Note that the T-ReCS N-band LR spectrum as published in [gonzalez-martin_dust_2013] exhibits ~ 25% higher flux levels than our photometry for unknown reasons and agrees with the IRS spectrum within the uncertainties. The difference between the arcsecond-scale and nuclear MIR SEDs is presumably caused by weak circum-nuclear star formation. The nuclear MIR emission of NGC 5506 could be further resolved with MIDI interferometric observations and was modelled as two components, one extending over \⪆10 pc, and a brighter one remaining unresolved (< 1 pc; [burtscher_diversity_2013]).

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Images

SEDs

MIR SED. The description of the symbols in all the SED plots (where present) is the following: Grey crosses and solid lines mark the Spitzer/IRAC, MIPS and IRS data. The colour coding of the other symbols is as follows: green for COMICS, magenta for Michelle, blue for T-ReCS and red for VISIR data. Darker-coloured solid lines mark spectra of the corresponding instrument. The black filled circles mark the nuclear 12 and 18 micron continuum emission estimate from the data (where present). The ticks on the top axis mark positions of common MIR emission lines, while the light grey horizontal bars mark wavelength ranges affected by the silicate 10 and 18 micron features.