Discovery of a spiral-host episodic radio galaxy

Hota, Ananda; Sirothia, S. K.; Ohyama, Youichi; Konar, C.; Kim, Suk; Rey, Soo-Chang; Saikia, D. J.; Croston, J. H.; Matsushita, Satoki

doi:10.1111/j.1745-3933.2011.01115.x

Cited by 97 publications

(111 citation statements)

References 40 publications

(61 reference statements)

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“…This redshift would mean that the physical size of the DRAGN associated with MCG+07-47-10 is significantly larger than 1 Mpc. We note that this would not necessarily be unusual for the class, as two previously identified spiral DRAGNS (Hota et al 2011;Bagchi et al 2014) show evidence of megaparsec structure. However, the host galaxy, MCG+07-47-10, would then have an optical size of approximately 100 kpc, which would be exceptionally large compared to similar analogues.…”

Section: Discussionmentioning

confidence: 98%

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Discovery of a low-luminosity spiral DRAGN

Mulcahy

Mao

Mitsuishi

et al. 2016

A&A

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Standard galaxy formation models predict that large-scale double-lobed radio sources, known as DRAGNs, will always be hosted by elliptical galaxies. In spite of this, in recent years a small number of spiral galaxies have also been found to host such sources. These so-called spiral DRAGNs are still extremely rare, with only ∼5 cases being widely accepted. Here we report on the serendipitous discovery of a new spiral DRAGN in data from the Giant Metrewave Radio Telescope (GMRT) at 322 MHz. The host galaxy, MCG+07-47-10, is a face-on late-type Sbc galaxy with distinctive spiral arms and prominent bulge suggesting a high black hole mass. Using WISE infra-red and GALEX UV data we show that this galaxy has a star formation rate of 0.16−0.75 M yr −1 , and that the radio luminosity is dominated by star-formation. We demonstrate that this spiral DRAGN has similar environmental properties to others of this class, but has a comparatively low radio luminosity of L 1.4 GHz = 1.12 × 10 22 W Hz −1 , two orders of magnitude smaller than other known spiral DRAGNs. We suggest that this may indicate the existence of a previously unknown low-luminosity population of spiral DRAGNS.

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Section: Discussionmentioning

confidence: 98%

“…Ledlow et al 2001;Hota et al 2011;Bagchi et al 2014;Mao et al 2015;Singh et al 2015). While the first three spiral DRAGN discoveries were serendipitous, Mao et al (2015) performed the first systematic search for these sources.…”

Section: Introductionmentioning

confidence: 99%

Discovery of a low-luminosity spiral DRAGN

Mulcahy

Mao

Mitsuishi

et al. 2016

A&A

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“…Furthermore, there is evidence for old "relic" radio lobes that span ∼1.3 Mpc, suggesting this radio source may be a giant radio galaxy 3 . Hota et al (2011) suggest that due to the unrelaxed nature of the galaxy cluster, and the evidence for recent star-formation, Speca may be accreting cold gas from the ICM. This would remove the need for a merger to feed the black hole.…”

Section: Radio Galaxies That Are Hosted By Spiralsmentioning

confidence: 99%

“…Speca (J1409-0302) was the second spiral galaxy found to host a large double-lobed radio source (Hota et al 2011). The host galaxy, at z = 0.138, is optically red yet also shows signs of recent star formation.…”

Section: Radio Galaxies That Are Hosted By Spiralsmentioning

confidence: 99%

J1649+2635: a grand-design spiral with a large double-lobed radio source

Mao

Owen

Duffin

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We report the discovery of a grand-design spiral galaxy associated with a double-lobed radio source. J1649+2635 (z = 0.0545) is a red spiral galaxy with a prominent bulge that it is associated with a L 1.4 GHz ∼10 24 W Hz −1 double-lobed radio source that spans almost 100 kpc. J1649+2635 has a black hole mass of M BH ∼ 3-7 × 10 8 M ⊙ and SFR ∼ 0.26 -2.6 M ⊙ year −1 . The galaxy hosts a ∼96 kpc diffuse optical halo, which is unprecedented for spiral galaxies. We find that J1649+2635 resides in an overdense environment with a mass of M dyn = 7.7 +7.9 −4.3 × 10 13 M ⊙ , likely a galaxy group below the detection threshold of the ROSAT All-Sky Survey. We suggest one possible scenario for the association of double-lobed radio emission from J1649+2635 is that the source may be similar to a Seyfert galaxy, located in a denser-than-normal environment. The study of spiral galaxies that host large-scale radio emission is important because although rare in the local Universe, these sources may be more common at high-redshifts.

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“…An other very recent example is the intermediate redshift disklike objects that shows spectacular radio lobe structures on scales of several 100 kpc suggestive of relicts Hota et al (2011). These rare cases of disk-dominated radio galaxies provide an excellent opportunity for studying the host galaxy properties and environmental effects that could be important for the triggering and/or evolution of their radio sources.…”

Section: Introductionmentioning

confidence: 99%

PKS 1814-637: a powerful radio-loud AGN in a disk galaxy

Morganti

Holt

Tadhunter

et al. 2011

A&A

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We present a detailed study of PKS 1814-637, a rare case of powerful radio source (P 5 GHz = 4.1 × 10 25 W Hz −1 ) hosted by a disk galaxy. Optical images have been used to model the host galaxy morphology confirming it to be dominated by a strong (and warped) disk component that is observed close to edge-on to the line of sight. This is the first radio galaxy found to reside in a disk dominated galaxy with radio luminosity equivalent to powerful FRII objects. At radio wavelengths, PKS 1814-637 is about 480 pc in diameter and it is classified as a compact steep spectrum (CSS) source; such sources are usually considered to be radio sources observed in the early stages of their evolution. However, the optical and mid-IR spectroscopic properties of PKS1814-637 show more in common with Seyfert galaxies than they do with radio galaxies, with the detection of H 2 , and PAH emission features, along with HI and silicate absorption features, providing evidence for a rich ISM which is likely to be related to the disk morphology of the host galaxy. We argue that the interaction between the radio plasma and the rich ISM in this and similar objects may have boosted their radio emission, allowing them to more easily enter flux limited samples of radio sources. In this case, PKS 1814-637 represents a type of "imposter": an intrinsically low power object that is selected in a radio flux limited sample because of the unusually efficient conversion of jet power into radio emission. This would make PKS 1814-637 an extreme example of the effects of jet-cloud interactions in galaxies containing a rich ISM, and perhaps a missing link between radio galaxies and radio-loud Seyfert galaxies. However, it is unlikely that jet-cloud interactions alone can account for the unusually powerful radio emission compared to Seyfert galaxies, and it is probable that the jet in PKS 1814-637 is also intrinsically more powerful than in typical Seyfert galaxies, perhaps due to a higher bulge and black hole mass. The estimated BH mass is indeed higher than the majority of Seyfert galaxies in the local Universe. We speculate that sources similar to PKS1814-637 are likely to be more common at high redshifts, because of the enhanced probability at earlier epochs of triggering radio sources in moderately massive bulges that are also gas-rich.

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Discovery of a spiral-host episodic radio galaxy

Cited by 97 publications

References 40 publications

Discovery of a low-luminosity spiral DRAGN

Discovery of a low-luminosity spiral DRAGN

J1649+2635: a grand-design spiral with a large double-lobed radio source

PKS 1814-637: a powerful radio-loud AGN in a disk galaxy

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