Kalloglyan and Tovmassian [57] have introduced a classification of galaxies judged solely on the degree of central concentration of galaxy images (Table I); examples of this system are also to be found in [56, 126, 136, 153, 154, 155, 186, 187, 188].
Keel and Weedman
[78] provided a survey
of 448 so-called
`bright-nuclei' (BN) galaxies of Type 4 and 5
(Table I), drawn from
the Byurakan master list
[3] of nuclear types for 711
galaxies. They
draw attention to 10 galaxies which have nuclei morphologically
resembling Seyfert galaxies, were originally defined by their optical
appearance
[168] but now have a
strict spectroscopic
classification
first suggested in a simpler form
[77], and then refined
and expanded upon by
[133,
134,
135] and outlined in
Table H. More
sophisticated diagnostic diagrams involving various optical
emission-line ratios can be found in
[197] and
[10], which
quantitatively discriminate between HII regions, starburst galaxies
(see [12]
for far infrared and optical models), HII galaxies,
narrow-line galaxies, LINER (low ionization nuclear emission region)
galaxies and Seyfert 2 galaxies. In this respect it is worth noting
that the N galaxies [120] now satisfy Seyfert's
original morphological
criteria as a separate class. Compilations of Seyfert galaxies and
related objects can be found in
[58,
89,
204,
205]. Early-type
galaxies with emission lines are brought together in
[13]. H emission-line strength surveys of
200 normal
galaxies [74] and 26
Virgo galaxies
[75].
Several surveys of Seyfert nuclei have discussed the morphology of the host galaxy [1, 7, 25, 172, 206]; other studies [45, 81, 82, 83, 132] have investigated the relation of Seyfert activity to their environment: Dahari [25] defines Interaction Classes for galaxies, in the context of nuclear activity, based on environmental criteria, given in Tables C, D, E, F; MacKenty [97] offers a simple two-way classification scheme (Table B) involving both the host morphology and the environment (in the form of a statement concerning interaction); [83] lists 113 galaxies in 15 Seyfert and 9 non-Seyfert groups and assigns Activity Classes (see Table G) to these galaxies.
Further environmental groupings have been assigned [20] for violently star-forming galaxies, as given in Table A.
Group | Description | Examples |
---|---|---|
1 | Morphologically normal galaxies with
nuclear starbursts. In all cases a companion is detected well within 1 Mpc projected separation, and ![]() | To 1004-296 UM 0499 Mrk 0710 |
2 | A burst of star formation appears to be located in a small companion, or corresponds to an HII region in the galaxy. | To 1116-325 UM 0501 Mrk 1315 |
3 | Magellanic irregular, or dwarf
irregular. Appears to be near other galaxies, and could be interacting. | To 1400-41 UM 0523 NGC 1487 |
4 | Small and compact. At least one massive galaxy is seen in the neighbourhood. | To 1147-283 UM 0462 Mrk 1318 |
5 | Small and compact. Nearby galaxies are not normal, being Magellanic irregulars or unclassified. | To
1924-416 UM 0160 II Zw 040 |
6 | Compact morphology and small size. Isolated (no companions within 500 km/sec or 1 Mpc projected separation). | To 1148-2020 UM 0439 NGC 5253 |
Class | Host Morphology Class | Interaction Class |
---|---|---|
0 | amorphous/unresolved | isolated |
1 | spiral | companion |
2 | bar and/or ring | companion is disturbed or at same redshift |
3 | peculiar or distorted | bridge, tail or jet |
IAC | Description | Example |
---|---|---|
1 | symmetric | Arp 027 |
2 | slightly asymmetric; diffuse extensions | Arp 026 |
3 | asymmetric, extended arm | Arp 222 |
4 | distorted; out of shape | Arp 224 |
5 | strongly distorted | Arp 220 |
6 | aftermath; severely distorted | Arp 157 |
IAC | Description | Example |
---|---|---|
3 | large separation, and no apparent contact | Arp 305 |
4 | large separation, but components are connected OR small separation, but no contact | Arp 314 Arp 271 |
5 | small separation, and evidence of contact | Arp 283 |
6 | galaxies overlap | Arp 166 |
IAC | Description | Example |
---|---|---|
2 | large separation, no contact | Arp 023 |
3 | large separation, but signs of connection | Arp 304 |
4 | small separation, but no contact OR small separation, and signs of contact | Arp 112 Arp 085 |
5 | companion overlaps parent galaxy | Arp 309 |
IAC | Description | Example |
---|---|---|
1 | large separation, no contact | . . . |
2 | large separation, but connected | Arp 024 |
3 | small separation, but no contact | Arp 290 |
4 | small separation, connected OR companion overlaps primary galaxy | Arp 082 Arp 239 |
5 | companion overlaps parent galaxy | Arp 309 |
Class | Spectrum |
---|---|
1 | Seyfert 1 or Seyfert 2 |
2 | Starburst nucleus with [OIII]![]() ![]() |
3 | H![]() ![]() ![]() |
4 | H![]() |
5 | H![]() |
6 | absorbtion lines only |
NET | Class | Description | Example |
---|---|---|---|
1 | Seyfert 1 | widths of the Balmer emission lines are much broader (several 1,000 km/sec) than the ``narrow'' forbidden line widths | NGC 4151 |
1.5 | Seyfert 1.5 Seyfert 1.8 Seyfert 1.9 | easily apparent, narrow H![]() narrow component of H ![]() ![]() broad H ![]() | Mrk 0006 NGC 2622 |
2 | Seyfert 2 | Balmer lines and forbidden lines have
similar widths, typically 500 - 1000 km s-1 ![]() ![]() ![]() ![]() ![]() ![]() | NGC 1068 |
2.5 | marginal Seyfert | ![]() ![]() ![]() ![]() ![]() ![]() | NGC 4388 NGC 7436 |
3 | LINER (Seyfert 3) | ![]() ![]() ![]() ![]() ![]() ![]() | NGC 3312 NGC 7393 |
4 | HII region | ![]() ![]() ![]() ![]() ![]() ![]() | NGC 4765 NGC 7253 |
5 | weak H![]() | NGC
3920 NGC 5410 | |
6 | no emission | EW H![]() | NGC 1143 |
7 | no emission | noisy or not observed when no nucleus is seen | NGC 0942 NGC 1347 |
Type | Description | Example |
---|---|---|
1 | No central condensation | NGC 4088 |
2 | Weak central condensation | NGC 5850 |
3 | Strong central condensation but not stellar | NGC 4442 |
4 | Stellar nucleus blending into nebulous background | NGC 1300 |
5 | Strongly stellar nucleus | NGC 3992 |