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Extended emission-line region

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.

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

[edit]

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

Name Host galaxy Image EELR Distance to nucleus (kpc) Date/Reference
MR 2251-178 30-50 1990[13]
Centaurus A

outer and inner filaments

7 & 16 1991[14]
IC 5063 22 1991[15]
3CR 368 45 1991[16]
3C 352 15.6 1992[17]
NGC 4151 1.16 1993[8]
NGC 3516 4 1995[7]
3C 273 14.4 1996[18]
PKS 2250–41 40-65 1997[19]
NGC 5643 1.8 1997[20]
PKS 2356–61 25 1998[21]
NGC 5256 7 2000[22]
NGC 4388 35 2002[23]
4C 37.43 20 2002[24]
3C 171 5 2003[25]
PKS 1932–46 100 2007[26]
3C 79 2008[5]
IC 2497 40[4] 2009[3]
3C 48 2009[1]
Mrk 1014 2009[1]
3C 249.1 2009[1]
Ton 616 2009[1]
Ton 202 2009[1]
PKS 2251+11 2009[1]
Mrk 78 16 2012[4]
SDSS J095559.88+395446.9 10 2012[4]
SDSS J100507.88+283038.5 13 2012[4]
IC 2637 11 2012[4]
NGC 3758 17 2012[4]
UGC 7342 38 2012[4]
NGC 5252 21 2012[4]
Mrk 273 19 2012[4]
Mrk 463 16 2012[4]
Teacup galaxy 18 2012[4]
SDSS J151004.01+074037.1 10 2012[4]
CGCG 077-117

(SDSS J152412.58+083241.2)

19 2012[4]
NGC 5972 33 2012[4]
Mrk 1498 21 2012[4]
Mrk 883 37 2012[4]
UGC 11185 11 2012[4]
SDSS J220141.64+115124.3 16 2012[4]
3C 305 2012[27]
3C 381 38 2013[28]
NGC 7252 4 2013[29]
PGC 043234 10 2016[30]
ShaSS 073 21 2018[31]
J023106−034513 30 2018[10]
J083823+015012 29 2018[10]
J090254+001116 10 2018[10]
J091113+032604 10 2018[10]
J092203−004443 13 2018[10]
J155143+434758 11 2018[10]
J162913+441442 15 2018[10]
J220347+020443 12 2018[10]
J220440+005232 8 2018[10]
J224027+004347 9 2018[10]
3C 17 10.5 2019[32]
3C 18 13 2019[32]
3C 33 6.3 2019[32]
3C 63 30.1 2019[32]
3C 318.1 11.7 2019[32]
3C 327 8.1 2019[32]
3C 353 12.7 2019[32]
3C 386 4.2 2019[32]
3C 403 11.3 2019[32]
3C 424 2.4 2019[32]
3C 442 3 2019[32]
3C 445 17 2019[32]
3C 458 80.2 2019[32]
3C 459 69 2019[32]
SDSS J002944.89+001011.1 2019[9]
SDSS J005754.03+012013.8 2019[9]
SDSS J083902.96+470756.3 2019[9]
Z 180–9 2019[9]
NGC 3341 2019[9]
UGC 6081 2019[9]
SDSS J120149.74-015327.5 2019[9]
SDSS J121418.25+293146.7 2019[9]
Arp 239 (NGC 5278/NGC 5279) 2019[9]
SDSS J135429.05+132757.2 2019[9]
Mrk 1172 14 2021[33]
NGC 235 26 2022[34]
NGC 5514 75 2022[34]
3C 98 6 2022[35]
3C 135 31.6 2022[35]
3C 180 59.8 2022[35]
3C 196.1 9.3 2022[35]
3C 198 32.6 2022[35]
3C 227 46.1 2022[35]
3C 300 17.2 2022[35]
2MASS J08001609+2928172 2023[36]
Z 119–12 2023[36]
2MASX J13020015+2746579 2023[36]
2MASS J08152577+3720258 2023[36]
2MASX J09515536+0329006 2023[36]
UGC 5941 2024[37]
Markarian 950 6.5 2024[38]
J1000+0234 >8.6 2024[12]
GSN 069 9.2 2024[39]
RXJ1301 2.8 2024[39]
eRO-QPE2 4.6 2024[39]

Notes

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

References

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