Extended emission-line region

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An extended emission-line region (EELR) is a giant interstellar cloud ionized by the radiation of an active galactic nucleus (AGN) inside a galaxy or photons produced by the shocks associated with the radio jets. [1] An EELR can appear as a resolved cloud in relative nearby galaxies and as narrow emission lines in more distant galaxies.

Contents

In this unified model of AGNs the EELRs should be thought as an extended version of the blue clouds labelled as "narrow line region". Emmaalexander unified agn.png
In this unified model of AGNs the EELRs should be thought as an extended version of the blue clouds labelled as "narrow line region".

EELRs were first discovered in radio galaxies. Usually the clouds emitting the narrow emission lines are restricted to a few kiloparsecs within the AGN, but some galaxies have narrow emission lines that extend a few kiloparsec to over 100 kiloparsecs. These clouds where therefore called extended emission-line regions (EELRs) and usually have a large doubly ionized oxygen [O III]/Hβ ratio, as well as a strong ionized helium He II/Hβ ratio (oxygen line at 5007 Å, helium line at 4686 Å). In some cases these EELRs show highly ionized species, such as calcium [Ca V] and iron [Fe VII] [Fe X]. [2] Another common highly ionized species is the emission of neon [Ne V] (main line at 3426 Å). [3] [4] This high level of ionization shows that the EELRs must be ionized by a mechanism related to the nucleus of the galaxy. HII regions do not show this high level of ionization. [2] The first [O III] images of EELRs were around galaxies, such as 3C 79, [5] 4C 37.43, [6] NGC 3516 [7] or NGC 4151. [8]

In 2009 a large cloud was discovered that had similar spectral features as EELRs, but had no ionizing AGN nearby. It was concluded that the nearby galaxy IC 2497 hosted an AGN in the past. Today this AGN faded into inactivity. The hard ionizing radiation did however need time to travel the thousands of lightyears towards a cloud, which would later become Hanny's Voorwerp. This makes Hanny's Voorwerp the first EELR associated with a fading AGN. Previously EELRs were commonly first discovered via spectroscopy and required high-resolution imaging to further resolve the EELRs. Hanny's Voorwerp was however discovered in broad band imaging from the Sloan Digital Sky Survey. [3] This prompted a search for more EELRs in broad-band imaging surveys by galaxy zoo volunteers, who also discovered Hanny's Voorwerp. EELRs are called "Voorwerpjes" by the galaxy zoo members. [4] EELRs that are ionized by the AGN of a companion galaxy were also discovered. This type of ionization is called cross-ionization. [9]

In broad-band images the [O III] emission lines usually lie at the g-band. The true color of an EELR would be dominated by the [O III] emission, which is a cyan color. In astronomical imaging slightly false-color images that transform g, r and i bands into RGB-images are more common. Sometimes the i-band is replaced with a z-band image. The EELRs appear as blue (g-band) objects in these survey images. Sometimes the H-alpha line is redshifted enough to lie at the i-band, which can make the EELR appear as a blue-violet object in these survey images. [4] Sometimes the [O III] is redshifted enough that this line overlaps with the r-band or i-band, which makes them green or red in survey images of the Hyper Suprime-Cam. [10] At around 0.1 < z < 0.38 the 5006.843 Å [O III] line is redshifted to the r-band and at 0.38 < z < 0.68 it is redshifted to the i-band. [note 1] A team of researchers detected a resolved EELR at a high redshift of 4.54 in a galaxy protocluster with JWST. [12]

Another related type of cloud is a extended narrow-line region (ENLR). The EELRs usually have dynamically chaotic structures and high velocities and are probably the result of mergers. ENLRs on the other hand follow the disk structure of the galaxy and have a low velocity. [10]

List of resolved EELRs

This is a list of EELRs with resolved [O III] images or other emission-lines

Name Host galaxyImage EELRDistance to nucleus (kpc)Date/Reference
MR 2251-178 MR 2251-178 MUSE.jpg 30-501990 [13]
Centaurus A

outer and inner filaments

 Centaurus A filaments (EELRs).jpg 7 & 161991 [14]
IC 5063 Mysterious Dark Rays (50651352623).jpg 221991 [15]
3CR 368451991 [16]
3C 35215.61992 [17]
NGC 4151 Seyfert galaxy NGC4151 (GL-2002-001035).jpg 1.161993 [8]
NGC 3516 NGC 3516.png 41995 [7]
3C 273 3C 273 MUSE.jpg 14.41996 [18]
PKS 2250–41 PKS 2250-41 legacy surveys.jpg 40-651997 [19]
NGC 5643 Center of galaxy NGC 5643.tif 1.81997 [20]
PKS 2356–61251998 [21]
NGC 5256 An ongoing cosmic collision.jpg 72000 [22]
NGC 4388 Eso0304c.jpg 352002 [23]
4C 37.43202002 [24]
3C 171 3C 171 cutout HST 05476 2l wfpc2 f702w pc sci.jpg 52003 [25]
PKS 1932–461002007 [26]
3C 79 3C 79 MUSE.jpg 2008 [5]
IC 2497 Hannys voorwerp.jpg 40 [4] 2009 [3]
3C 48 2009 [1]
Mrk 1014 Mrk 1014 MUSE.jpg 2009 [1]
3C 249.1 2009 [1]
Ton 6162009 [1]
Ton 2022009 [1]
PKS 2251+112009 [1]
Mrk 78 Mrk 78 (50838249333).png 162012 [4]
SDSS J095559.88+395446.9 SDSS J0955+3954.jpg 102012 [4]
SDSS J100507.88+283038.5 SDSS J1005+2830 legacy surveys.jpg 132012 [4]
IC 2637 112012 [4]
NGC 3758 NGC 3758 MUSE 2.jpg 172012 [4]
UGC 7342 Heic1507e.jpg 382012 [4]
NGC 5252 Heic1507f.jpg 212012 [4]
Mrk 273 Mrk 273 Hubble.jpg 192012 [4]
Mrk 463 Mrk 463 MUSE.jpg 162012 [4]
Teacup galaxy The Teacup Galaxy SDSS 1430.jpg 182012 [4]
SDSS J151004.01+074037.1 Hs-2015-13-d-large web.jpg 102012 [4]
CGCG 077-117

(SDSS J152412.58+083241.2)

 CGCG 077-117 MUSE.jpg 192012 [4]
NGC 5972 NGC 5972.jpg 332012 [4]
Mrk 1498 Hs-2015-13-g-large web.jpg 212012 [4]
Mrk 883 Mrk 883 legacy surveys.jpg 372012 [4]
UGC 11185 Heic1507h.jpg 112012 [4]
SDSS J220141.64+115124.3 Hs-2015-13-i-large web.jpg 162012 [4]
3C 305 IC 1065 (3C 305) Chandra.jpg 2012 [27]
3C 381382013 [28]
NGC 7252 42013 [29]
PGC 043234102016 [30]
ShaSS 073 An echo of light ShaSS 073, ShaSS 622, ShaSS 622-073 (cropped).jpg 212018 [31]
J023106−034513302018 [10]
J083823+015012292018 [10]
J090254+001116102018 [10]
J091113+032604102018 [10]
J092203−004443132018 [10]
J155143+434758112018 [10]
J162913+441442152018 [10]
J220347+020443122018 [10]
J220440+00523282018 [10]
J224027+00434792018 [10]
3C 1710.52019 [32]
3C 18132019 [32]
3C 336.32019 [32]
3C 6330.12019 [32]
3C 318.111.72019 [32]
3C 3278.12019 [32]
3C 35312.72019 [32]
3C 3864.22019 [32]
3C 40311.32019 [32]
3C 4242.42019 [32]
3C 44232019 [32]
3C 445172019 [32]
3C 458 3C 458 MUSE.jpg 80.22019 [32]
3C 459692019 [32]
SDSS J002944.89+001011.12019 [9]
SDSS J005754.03+012013.8 SDSS J0057+0120.jpg 2019 [9]
SDSS J083902.96+470756.32019 [9]
Z 180–92019 [9]
NGC 3341 NGC 3341 MUSE.jpg 2019 [9]
UGC 6081 UGC 6081 legacy surveys.jpg 2019 [9]
SDSS J120149.74-015327.52019 [9]
SDSS J121418.25+293146.7 SDSS J1214+2931 Hubble.jpg 2019 [9]
Arp 239 (NGC 5278/NGC 5279) NGC 5278 79 Arp239 SDSS2.jpg 2019 [9]
SDSS J135429.05+132757.22019 [9]
Mrk 1172142021 [33]
NGC 235 262022 [34]
NGC 5514 752022 [34]
3C 9862022 [35]
3C 13531.62022 [35]
3C 18059.82022 [35]
3C 196.19.32022 [35]
3C 19832.62022 [35]
3C 227 3C 227 MUSE.jpg 46.12022 [35]
3C 30017.22022 [35]
2MASS J08001609+29281722023 [36]
Z 119–122023 [36]
2MASX J13020015+27465792023 [36]
2MASS J08152577+37202582023 [36]
2MASX J09515536+03290062023 [36]
UGC 5941 2024 [37]
Markarian 9506.52024 [38]
J1000+0234 J1000+0234 EELR.jpg >8.62024 [12]

Notes

  1. ↑ Calculated with the formula z=(λobserve-λemit)/λemit and the transition of SDSS filters from Figure 2 in Smith et al. 2002 [11]

Related Research Articles

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<span class="mw-page-title-main">Hanny's Voorwerp</span> Astronomical object appearing as a bright blob, discovered by Hanny van Arkel

Hanny's Voorwerp is a type of astronomical object called a quasar ionization echo. It was discovered in 2007 by Dutch schoolteacher Hanny van Arkel while she was participating as a volunteer in the Galaxy Zoo project, part of the Zooniverse group of citizen science websites. Photographically, it appears as a bright blob close to spiral galaxy IC 2497 in the constellation Leo Minor.

<span class="mw-page-title-main">Hercules A</span>

Hercules A is a bright astronomical radio source in the constellation Hercules corresponding to the galaxy 3C 348.

<span class="mw-page-title-main">Green bean galaxy</span> Very rare astronomical objects that are thought to be quasar ionization echos

Green bean galaxies (GBGs) are very rare astronomical objects that are thought to be quasar ionization echos. They were discovered by Mischa Schirmer and colleagues R. Diaz, K. Holhjem, N.A. Levenson, and C. Winge. The authors report the discovery of a sample of Seyfert-2 galaxies with ultra-luminous galaxy-wide narrow-line regions (NLRs) at redshifts z=0.2-0.6.

<span class="mw-page-title-main">NGC 3862</span> Galaxy in the constellation Leo

NGC 3862 is an elliptical galaxy located 300 million light-years away in the constellation Leo. Discovered by astronomer William Herschel on April 27, 1785, NGC 3862 is an outlying member of the Leo Cluster.

<span class="mw-page-title-main">NGC 3860</span> Spiral galaxy in the constellation Leo

NGC 3860 is a spiral galaxy located about 340 million light-years away in the constellation Leo. NGC 3860 was discovered by astronomer William Herschel on April 27, 1785. The galaxy is a member of the Leo Cluster and is a low-luminosity AGN (LLAGN). Gavazzi et al. however classified NGC 3860 as a strong AGN which may have been triggered by a supermassive black hole in the center of the galaxy.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

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<span class="mw-page-title-main">Teacup galaxy</span> Low redshift quasar in the constellation Boötes

The Teacup galaxy, also known as the Teacup AGN or SDSS J1430+1339 is a low redshift type 2 quasar, showing an extended loop of ionized gas resembling a handle of a teacup, which was discovered by volunteers of the Galaxy Zoo project and labeled as a Voorwerpje.

<span class="mw-page-title-main">4C+55.16</span> Seyfert 2 galaxy in the constellation Ursa Major

4C+55.16 is an elliptical galaxy, classified type E, located in Ursa Major. The galaxy lies about 2.84 billion light-years from Earth, which means given its apparent dimensions, 4C+55.16 is approximately 445,000 light-years across making it a type-cD galaxy. It is the brightest cluster galaxy (BCG) in a cluster bearing its same name and a part of the galaxy cluster called WHL J083454.9+553421.

<span class="mw-page-title-main">4C +29.30</span> Galaxy in the constellation Cancer

4C +29.30 is an elliptical galaxy located in Cancer constellation. Its redshift is 0.064840 which corresponds to a light travel time of 850 million light-years from Earth. It is a wide-angled tailed radio galaxy (WAT) and a Seyfert galaxy.

<span class="mw-page-title-main">IRAS 09104+4109</span> Galaxy in the constellation Lynx

IRAS 09104+4109 is a galaxy located in the constellation Lynx. With a redshift of 0.440797, the light travel time for this galaxy, corresponds to 4.8 billion light-years from Earth. It is the brightest cluster galaxy in CDGS 25, also known as WHL J091345.5+405628 and a notable, unique ultraluminous infrared galaxy.

<span class="mw-page-title-main">4C +09.17</span> Quasar in the constellation Orion

4C +09.17 is a quasar located in the constellation Orion. With a redshift of 2.108300, the object is located 10.6 billion light years from Earth and presents an extragalactic astrophysical jet morphology.

<span class="mw-page-title-main">PKS 1345+125</span> Galaxy merger in the constellation Boötes

PKS 1345+125 known as PKS 1345+12 and 4C +12.50, is an ultraluminous infrared galaxy (ULIG) with an active galactic nucleus, located in the constellation Boötes. With a redshift of 0.121740, the galaxy is located 1.7 billion light-years from Earth.

<span class="mw-page-title-main">PKS 1402-012</span> Quasar in the constellation of Virgo

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<span class="mw-page-title-main">4C +03.10</span> Quasar in the constellation Orion

4C +03.10 also known as PKS 0505+03 and OG +008, is a quasar located in the constellation of Orion. At a redshift of 2.46, the object is located 10.6 billion light-years away from Earth.

<span class="mw-page-title-main">Abell 697 BCG</span> Brightest cluster galaxy in the constellation Lynx

Abell 697 BCG, also known as PGC 2079433, is a massive type-cD elliptical galaxy residing as the brightest cluster galaxy in Abell 697 galaxy cluster. It is located in the constellation of Lynx and has a redshift of 0.28, meaning the galaxy is located 3.5 billion light-years away from Earth.

<span class="mw-page-title-main">2MASX J17201001+2637317</span>

2MASX J17201001+2637317 also known as PGC 1782937, is a massive type-cD elliptical galaxy located in the constellation of Hercules. With redshift of 0.16, the galaxy is located 2.4 billion light-years from Earth and the brightest cluster galaxy in the galaxy cluster, RX J1720.1+2638.

<span class="mw-page-title-main">Abell 68</span> Galaxy cluster in the constellation Pisces

Abell 68 is massive and rich galaxy cluster located in the constellation of Pisces with a projected co-moving distance of approximately 1124.6 Mpc or 3.668 billion light-years away from Earth. The cluster is especially notable for its gravitational lensing and was first discovered by George O. Abell in 1958.

<span class="mw-page-title-main">PG 1543+489</span> Quasar in the constellation of Boötes

PG 1543+489, also known as QSO B1544+4855 and PGC 2325245, is a quasar located in the constellation of Boötes. At the redshift of 0.399, the object is located 4.5 billion light-years away from Earth. It was first discovered in 1983, by researchers who presented 114 objects in the Palomar-Green bright quasar survey, as one of the best studied samples of active galactic nuclei (AGN).

<span class="mw-page-title-main">4C +26.42</span> Elliptical galaxy in the constellation of Boötes

4C +26.42 is an elliptical galaxy located in the constellation of Boötes. It has a redshift of 0.063, estimating the galaxy to be located 863 million light-years from Earth. It has an active galactic nucleus and is the brightest cluster galaxy (BCG) in Abell 1795, an X-ray luminous rich cluster (LX 1045 ergs s-1), with an estimated cooling-flow rate of 300 M yr-1.

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  31. ↑ Merluzzi, Paola; Busarello, Giovanni; Dopita, Michael A.; Thomas, Adam D.; Haines, Chris P.; Grado, Aniello; Limatola, Luca; Mercurio, Amata (2018-01-01). "An Interacting Galaxy Pair at the Origin of a Light Echo". The Astrophysical Journal. 852 (2): 113. arXiv: 1801.01005 . Bibcode:2018ApJ...852..113M. doi: 10.3847/1538-4357/aa9fff . ISSN   0004-637X.
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  34. 1 2 Keel, William C.; Moiseev, Alexei; Kozlova, D. V.; Ikhsanova, A. I.; Oparin, D. V.; Uklein, R. I.; Smirnova, A. A.; Eselevich, M. V. (2022-03-01). "The TELPERION survey for distant [O III] clouds around luminous and hibernating AGN". Monthly Notices of the Royal Astronomical Society. 510 (3): 4608–4625. arXiv: 2112.07084 . Bibcode:2022MNRAS.510.4608K. doi: 10.1093/mnras/stab3656 . ISSN   0035-8711.
  35. 1 2 3 4 5 6 7 Balmaverde, B.; Capetti, A.; Baldi, R. D.; Baum, S.; Chiaberge, M.; Gilli, R.; Jimenez-Gallardo, A.; Marconi, A.; Massaro, F.; Meyer, E.; O'Dea, C.; Speranza, G.; Torresi, E.; Venturi, G. (2022-06-01). "The MURALES survey. VI. Properties and origin of the extended line emission structures in radio galaxies". Astronomy and Astrophysics. 662: A23. arXiv: 2204.00528 . Bibcode:2022A&A...662A..23B. doi:10.1051/0004-6361/202142823. ISSN   0004-6361.
  36. 1 2 3 4 5 French, K. Decker; Earl, Nicholas; Novack, Annemarie B.; Pardasani, Bhavya; Pillai, Vismaya R.; Tripathi, Akshat; Verrico, Margaret E. (2023-06-01). "Fading AGNs in Poststarburst Galaxies". The Astrophysical Journal. 950 (2): 153. arXiv: 2304.10419 . Bibcode:2023ApJ...950..153F. doi: 10.3847/1538-4357/acd249 . ISSN   0004-637X.
  37. ↑ Keel, William; Moiseev, Alexei; Uklein, Roman; Smirnova, Aleksandrina (2024-03-01), The TELPERION survey for extended emission regions around AGN: a strongly-interacting and merging galaxy sample, arXiv: 2403.04898 , retrieved 2024-03-29
  38. ↑ Wevers, Thomas; French, K. Decker (June 2024), "Extended emission line regions in post-starburst galaxies hosting tidal disruption events", The Astrophysical Journal, 969 (1): L17, arXiv: 2406.02674 , Bibcode:2024ApJ...969L..17W, doi: 10.3847/2041-8213/ad5725
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