A search for QSOs in the fields of nearby galaxies - II. NGC 55, 253, 300 and 5364

Monk, A. S.; Penston, M. V.; Blades, J. C.

doi:10.1093/mnras/222.4.787

Cited by 14 publications

(19 citation statements)

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“…The nuclei that are host to the detected maser emission are spectroscopically classified as Seyfert 2 or LINER in all but two cases (Table 1). Ambiguity remains in the case of NGC 0613, which is listed as a possible Seyfert by Veron-Cetty & Veron (1986), and in the case of NGC 0235A, which is classified as Seyfert 2 by Monk et al (1986) but as Seyfert 1 by Maia et al (1987). There is some indication of a broad component in Hα in the optical spectrum presented by Maia et al (1987) (the Monk et al (1986) spectrum does not cover the wavelength of Hα).…”

Section: Resultsmentioning

confidence: 97%

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Discovery of Water Maser Emission in Eight AGNs with 70 m Antennas of NASA’s Deep Space Network

Kondratko

Greenhill

Moran

et al. 2006

ApJ

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We report the discovery of water maser emission in eight active galactic nuclei (AGN) with the 70-m NASA Deep Space Network (DSN) antennas at Tidbinbilla, Australia and Robledo, Spain. The positions of the newly discovered masers, measured with the VLA, are consistent with the optical positions of the host nuclei to within 1σ (0. ′′ 3 radio and 1. ′′ 3 optical) and most likely mark the locations of the embedded central engines. The spectra of two sources, NGC 3393 and NGC 5495, display the characteristic spectral signature of emission from an edge-on accretion disk, with orbital velocities of ∼ 600 and ∼ 400 km s −1 , respectively. In a survey with DSN facilities of 630 AGN selected from the NASA Extragalactic Database, we have discovered a total of 15 water maser sources. The resulting incidence rate of maser emission among nearby (v sys < 7000 km s −1) Seyfert 1.8 − 2.0 and LINER systems is ∼ 10% for a typical rms noise level of ∼ 14 mJy over 1.3 km s −1 spectral channels. As a result of this work, the number of nearby AGN (v sys < 7000 km s −1) observed with < 20 mJy rms noise has increased from 130 to 449.

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Section: Resultsmentioning

confidence: 97%

“…Type (a) α 2000 (b) δ 2000 (b) vsys (c) log 10 LH 2 O (d) -Cetty & Veron (1986), NGC 4293 is listed as LINER by Ho et al (1997a), while NGC 0235A is classified as Seyfert 1 by Maia et al (1987) but as Seyfert 2 by Monk et al (1986). Refer to the text for the discussion of the ambiguity in NGC 0235A spectral classification.…”

Section: Galaxymentioning

confidence: 99%

Discovery of Water Maser Emission in Eight AGNs with 70 m Antennas of NASA’s Deep Space Network

Kondratko

Greenhill

Moran

et al. 2006

ApJ

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“…• 06 04.8 , 2MASS, Cutri et al 2003) detected for the first time in the ESO B Southern Sky Survey (Monk et al 1986). It has strong, broad permitted optical emission lines (e.g., FWHM(H β ) = 4 700 ± 160 km s −1 , Grupe et al 1999), which led to it being described as a Broad-Line Seyfert 1 AGN.…”

Section: Introductionmentioning

confidence: 96%

An intense and broad Fe K_α line observed in the X-ray luminous quasar Q 0056-363 with XMM-Newton

Porquet

Reeves

2003

A&A

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Abstract. We present an XMM-Newton observation of the radio-quiet quasar Q0056-363 (z = 0.162). This is the first time that this quasar is observed in the hard X-ray range (above 2 keV). We find that Q0056-363 is a powerful X-ray quasar, with a 0.3-12 keV unabsorbed luminosity of about 1.2 × 10 45 erg s −1 with the largest part (∼67%) emitted below 2 keV. The spectrum reveals a large featureless soft X-ray excess below 2 keV and a strong broad Fe K α line at 6.4 keV (in the quasar frame).The Fe K α line is due to low to moderate ionization states of iron (i.e.,

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“…Not only is access to the satellite limited due to high demand, but the telescope's modest mirror size restricts spectroscopic observations to only the brightest objects. Nevertheless, it was always expected prior to its launch that HST would probe galaxy halos along more than single sightlines (e.g., Monk et al 1986), and indeed some attempts were made with the first generation of HST spectrographs (e.g., Norman et al 1996;Bowen et al 1997). Significant progress has been made in the last few years, however, as COS has enabled observations of the fainter QSOs that constitute a higher surface density on the sky.…”

Section: Introductionmentioning

confidence: 99%

The Structure of the Circumgalactic Medium of Galaxies: Cool Accretion Inflow Around NGC 1097*

Bowen

Chelouche

Jenkins

et al. 2016

ApJ

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We present Hubble Space Telescope far-UV spectra of four QSOs whose sightlines pass through the halo of NGC 1097 at impact parameters of ρ = 48-165 kpc. NGC 1097 is a nearby spiral galaxy that has undergone at least two minor merger events, but no apparent major mergers, and is relatively isolated with respect to other nearby bright galaxies. This makes NGC 1097 a good case study for exploring baryons in a paradigmatic bright-galaxy halo. Lyα absorption is detected along all sightlines and Si IIIλ1206 is found along the three sightlines with the smallest ρ; metal lines of C II, Si II, and Si IV are only found with certainty toward the innermost sightline. The kinematics of the absorption lines are best replicated by a model with a disk-like distribution of gas approximately planar to the observed 21 cm H I disk, which is rotating more slowly than the inner disk, and into which gas is infalling from the intergalactic medium. Some part of the absorption toward the innermost sightline may arise either from a smallscale outflow or from tidal debris associated with the minor merger that gives rise to the well known "dog-leg" stellar stream that projects from NGC 1097. When compared to other studies, NGC 1097 appears to be a "typical" absorber, although the large dispersion in absorption line column density and equivalent width in a single halo goes perhaps some way toward explaining the wide range of these values seen in higher-z studies.

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A search for QSOs in the fields of nearby galaxies - II. NGC 55, 253, 300 and 5364

Cited by 14 publications

References 0 publications

Discovery of Water Maser Emission in Eight AGNs with 70 m Antennas of NASA’s Deep Space Network

Discovery of Water Maser Emission in Eight AGNs with 70 m Antennas of NASA’s Deep Space Network

An intense and broad Fe K_α line observed in the X-ray luminous quasar Q 0056-363 with XMM-Newton

The Structure of the Circumgalactic Medium of Galaxies: Cool Accretion Inflow Around NGC 1097*

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A search for QSOs in the fields of nearby galaxies - II. NGC 55, 253, 300 and 5364

Cited by 14 publications

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Discovery of Water Maser Emission in Eight AGNs with 70 m Antennas of NASA’s Deep Space Network

Discovery of Water Maser Emission in Eight AGNs with 70 m Antennas of NASA’s Deep Space Network

An intense and broad Fe Kα line observed in the X-ray luminous quasar Q 0056-363 with XMM-Newton

The Structure of the Circumgalactic Medium of Galaxies: Cool Accretion Inflow Around NGC 1097*

Contact Info

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Resources

About

An intense and broad Fe K_α line observed in the X-ray luminous quasar Q 0056-363 with XMM-Newton