Third Reference Catalogue of Bright Galaxies

Vaucouleurs, G. de; Vaucouleurs, A. de; Corwin, H. G.; Buta, Ronald J.; Paturel, G.; Fouqué, P.

doi:10.1007/978-1-4757-4360-9_1

Cited by 699 publications

(864 citation statements)

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“…The Galactic extinction toward NGC 4278 is 0.11 mag (de Vaucouleurs et al 1991). The same value is derived using the Galactic hydrogen column density and applying the equations E(B−V) = NH/(5.8 × 10 21 ) mag and A V /E(B−V) = 3.1.…”

Section: Spectral Energy Distributionmentioning

confidence: 80%

X-ray and multiwavelength view of NGC 4278

Younes

Porquet

Sabra

et al. 2010

A&A

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Context. The emission mechanism responsible for the bulk of energy from radio to X-rays in low ionization emission line regions (LINERs) and low luminosity active galactic nuclei (LLAGN) has been long debated. Based on UV to X-ray and radio to UV flux ratios, some argue that LINERs/LLAGN are a scaled-down version of their more luminous predecessors Seyfert galaxies. Others, based on the lack of X-ray short (hours) time-scale variability, the non detection of an iron line at 6.4 keV, and the faint UV emission compared to typical AGNs, suggest the truncation of the classical thin accretion disk in the inner regions of the AGN where a radiatively inefficient accretion flow (RIAF) structure forms. Aims. We investigate the LINER-Seyfert connection by studying the unabsorbed LINER galaxy NGC 4278 that accretes at a low rate (L bol/Edd ∼ 7 × 10 −6 ) but exhibits a broad Hα line, and a point-like nucleus in radio, optical, UV and X-rays. Methods. We analyzed one XMM-Newton and seven Chandra X-ray observations of NGC 4278 spread over a three year period, allowing the study of the X-ray variability at different time-scales (hours, months, years). We also examined the radio to X-ray spectral energy distribution to constrain the accretion mode in the nucleus of NGC 4278. Results. Long time-scale (months) variability is observed where the flux increased by a factor of ∼3 on a time-scale of a few months and by a factor of 5 between the faintest and the brightest observation separated by ∼3 years. During the XMM-Newton observation, where the highest flux level is detected, we found a 10% flux increase on a short time-scale of a few hours, while the light curves for the different Chandra observations do not show short time-scale (minutes to hours) variability. A combination of an absorbed power law (N H ≈ 10 20 cm −2 , Γ = 2.2 +0.1 −0.2 ) plus a thermal component (kT ≈ 0.6 keV) were able to fit the Chandra spectra. The XMM-Newton spectra, where the highest X-ray flux is detected, are well fitted with an absorbed power-law with no need for a thermal component as the emission from the power-law component is dominant. The power-law photon index is ∼2.1 and the hydrogen column density is of the order of 10 20 cm −2 . Neither a narrow nor a broad Fe Kα emission line at 6.4 keV are detected with a 22 eV and 118 eV upper limits derived on their equivalent widths. We derive optical fluxes from archival HST ACS observations and detected optical variability on time-scales of years. For the first time for this source, thanks to the optical/UV monitor on board XMM-Newton, we obtained simultaneous UV and X-ray flux measurements. We constructed SEDs based on simultaneous or quasi simultaneous observations and compared them to LINER, radio-loud, and radio-quiet quasar SEDs. We find that at a low X-ray flux the NGC 4278 SED resembles that of typical LINER sources where the radio to X-ray emission can be considered as originating from a jet and/or RIAF, whereas at a high X-ray flux, NGC 4278 SED is more like a low luminosity Seyfert SED...

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Section: Spectral Energy Distributionmentioning

confidence: 80%

X-ray and multiwavelength view of NGC 4278

Younes

Porquet

Sabra

et al. 2010

A&A

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“…Following Choi et al (2010), we used the Two-degree Field Galaxy Redshift Survey (2dFGRS, Colless et al 2001Colless et al , 2003, the Two Micron All Sky Survey (2MASS, Jarrett et al 2003;Skrutskie et al 2006) Redshift Survey (2MRS, Huchra et al 2012), and the Third Reference Catalogue of Bright Galaxies (RC3, de Vaucouleurs et al 1991;Corwin et al 1994) to complement the SDSS photometric objects with redshifts measured by one of the previously mentioned surveys. The addition of these objects improves the completeness for bright nearby objects and for objects in relatively nearby high-density regions (e.g.…”

Section: Spectroscopically Complemented Galaxy Samplementioning

confidence: 99%

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Tempel

Tamm

Gramann

et al. 2014

A&A

219

487

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We provide flux-and volume-limited galaxy group and cluster catalogues based on the spectroscopic sample of the galaxies of SDSS data release 10. We used a modified friends-of-friends method with a variable linking length in the transverse and radial directions to identify as many realistic groups as possible. The flux-limited catalogue incorporates galaxies down to m r = 17.77 mag. It includes 588 193 galaxies and 82 458 groups. The volume-limited catalogues are complete for absolute magnitudes down to M r,lim = −18.0, −18.5, −19.0, −19.5, −20.0, −20.5, and −21.0; the completeness is achieved within different spatial volumes. Our analysis shows that flux-and volume-limited group samples are well compatible, especially for the larger groups/clusters. Dynamical mass estimates based on radial velocity dispersions and group extent in the sky were added to the extracted groups.

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“…Based on IC 1459's dynamically inferred black hole mass of 3 − 12 × 10 8 M , Verdoes Kleijn et al (2000) estimate a total galaxy mass of ∼3 ×10 11 M (all quoted mass estimates are adjusted to our adopted distance). Using dynamic modelling of the HST data they measure a systemic velocity of v sys = 1783 ± 10 km s −1 , of the ionised gas in IC 1459, ∼90 km s −1 higher than IC 1459's optical velocity of 1691 ± 18 km s −1 (de Vaucouleurs et al 1991). A narrow (35 km s −1 ) 12 CO(1-0) line emission towards IC 1459 at v sys = 1782 km s −1 was detected by Bettoni et al (2001).…”

Section: The Ic 1459 Galaxy Groupmentioning

confidence: 99%

H i debris in the IC 1459 galaxy group

Saponara

Koribalski

Benaglia

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present H i synthesis imaging of the giant elliptical galaxy IC 1459 and its surroundings with the Australia Telescope Compact Array (ATCA). Our search for extended H i emission revealed a large complex of H i clouds near IC 1459, likely the debris from tidal interactions with neighbouring galaxies. The total H i mass (∼ 10 9 M ) in the detected clouds spans 250 kpc from the north-east of the gas-rich spiral NGC 7418A to the south-east of IC 1459. The extent and mass of the H i debris, which shows rather irregular morphology and kinematics, are similar to those in other nearby groups. Together with H i clouds recently detected near two other IC 1459 group members, namely IC 5270 and NGC 7418, using Phased-Array Feeds (PAFs) on the Australian Square Kilometer Array Pathfinder (ASKAP), the detected debris make up a significant fraction of the group's intergalactic medium.

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Third Reference Catalogue of Bright Galaxies

Cited by 699 publications

References 0 publications

X-ray and multiwavelength view of NGC 4278

X-ray and multiwavelength view of NGC 4278

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

H i debris in the IC 1459 galaxy group

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