Dorado Group: Difference between revisions
Spacepotato (talk | contribs) Add "the" |
m Open access bot: doi added to citation with #oabot. |
||
(43 intermediate revisions by 31 users not shown) | |||
Line 1: | Line 1: | ||
{{Galaxy cluster |
{{Short description|Galaxy cluster in the constellation Dorado}} |
||
{{Galaxy cluster |
|||
| name = Dorado Group |
| name = Dorado Group |
||
| image = |
| image = [[Image:Sig05-013 small.jpg|300px]] |
||
| caption = NGC 1566, one of the brightest members of the Dorado Group ([[Spitzer Space Telescope]] image) |
|||
| epoch = [[J2000]] |
| epoch = [[J2000]] |
||
| ra = {{RA|04|17|03.9}}<ref name="ned">{{ |
| ra = {{RA|04|17|03.9}}<ref name="ned">{{Citation |
||
| title=NASA/IPAC Extragalactic Database |
| title=NASA/IPAC Extragalactic Database |
||
| work=Results for Dorado Group and various galaxies |
| work=Results for Dorado Group and various galaxies |
||
| url=http://nedwww.ipac.caltech.edu/ |
| url=http://nedwww.ipac.caltech.edu/ |
||
| |
| access-date=2008-06-26}}</ref> |
||
| dec = {{DEC|-56|07|43}}<ref name="ned" /> |
| dec = {{DEC|-56|07|43}}<ref name="ned" /> |
||
| constellation = [[Dorado]] |
| constellation = [[Dorado]] |
||
Line 13: | Line 16: | ||
| brightest_member = [[NGC 1566]] |
| brightest_member = [[NGC 1566]] |
||
| other_names = Shk 18,<ref name="Carrascoetal2001" /> G16,<ref name="Carrascoetal2001" /><ref name="Fergusonetal1990" /> HG3,<ref name="Carrascoetal2001">{{citation |
| other_names = Shk 18,<ref name="Carrascoetal2001" /> G16,<ref name="Carrascoetal2001" /><ref name="Fergusonetal1990" /> HG3,<ref name="Carrascoetal2001">{{citation |
||
| title = The Dwarf Galaxy Population of the Dorado Group Down to M<sub>V</sub>~ |
| title = The Dwarf Galaxy Population of the Dorado Group Down to M<sub>V</sub>~−11 |
||
| |
|author1=Carrasco, Eleazar R. |author2=Mendes de Oliveira, Cláudia |author3=Infante, Leopoldo |author4=Bolte, Michael | journal = The Astronomical Journal |
||
| journal = The Astronomical Journal |
|||
| volume = 121 |
| volume = 121 |
||
| issue = 1 |
| issue = 1 |
||
| pages = |
| pages = 148–168 |
||
| year = 2001 |
|||
| date = January 2001 |
| date = January 2001 |
||
| |
| bibcode = 2001AJ....121..148C |
||
| doi = 10.1086/318035 |
| doi = 10.1086/318035 |
||
}}</ref> MC13,<ref name="Maiaetal1989" /> and NGC 1566 Group<ref name="Kilbornetal2005" /> |
|arxiv = astro-ph/0010076 |s2cid=1348985 }}</ref> MC13,<ref name="Maiaetal1989" /> and NGC 1566 Group<ref name="Kilbornetal2005" /> |
||
}} |
}} |
||
The '''Dorado Group''' is a loose [[Galaxy groups and clusters|concentration of galaxies]]<ref name="Carrascoetal2001" /> containing both [[spiral galaxy|spiral]]s and [[elliptical galaxy|elliptical]]s.<ref name="Fergusonetal1990">{{citation | bibcode = 1990AJ....100....1F | title = Population studies in groups and clusters of galaxies. III – A catalog of galaxies in five nearby groups | date = July 1990 | last1 = Ferguson | first1 = Henry C. | last2 = Sandage | first2 = Allan | author-link2 = Allan Sandage | journal = Astronomical Journal | issn = 0004-6256 | volume = 100 | pages = 1–31 | doi = 10.1086/115486| doi-access = free }}</ref> It is generally considered a 'galaxy group' but may approach the size of a 'galaxy cluster'.<ref name="Firthetal2006" /> It lies primarily in the southern constellation [[Dorado]] and is one of the richest galaxy groups of the [[Southern Hemisphere]].<ref name="Laurikainenetal2006">{{citation | bibcode = 2006AJ....132.2634L | title = The Near-infrared S0 Survey III: Morphology of 15 Southern Early-Type Disk Galaxies | date = December 2006 | journal = The Astronomical Journal | volume = 132 | issue = 6 | pages = 2634–2652 | doi = 10.1086/508810 |author1=Laurikainen, Eija |author2=Salo, Heikki |author3=Buta, Ronald |author4=Knapen, Johan |author5=Speltincx, Tom |author6=Block, David |arxiv = astro-ph/0609343 | s2cid = 16856632 }}</ref> [[Gérard de Vaucouleurs]] was the first to identify it in 1975 as a large complex nebulae II in the Dorado region,<ref name="Carrascoetal2001" /> designating it as G16.<ref name="Fergusonetal1990" /> |
|||
The '''Dorado Group''' is a loose [[Galaxy groups and clusters|concentration of galaxies]]<ref name="Carrascoetal2001" /> containing both [[spiral galaxy|spiral]]s and [[elliptical galaxy|elliptical]]s.<ref name="Fergusonetal1990">{{citation |
|||
| url = http://adsabs.harvard.edu/abs/1990AJ....100....1F |
|||
| title = Population studies in groups and clusters of galaxies. III - A catalog of galaxies in five nearby groups |
|||
| year = 1990 |
|||
| date = July 1990 |
|||
| last1 = Ferguson |
|||
| first1 = Henry C. |
|||
| last2 = Sandage |
|||
| first2 = Allan |
|||
| authorlink2 = Allan Sandage |
|||
| journal = Astronomical Journal |
|||
| issn = 0004-6256 |
|||
| volume = 100 |
|||
| pages = 1–31 |
|||
| doi = 10.1086/115486 |
|||
}}</ref> It is generally considered a 'galaxy group' but may approach the size of a 'galaxy cluster'.<ref name="Firthetal2006" /> It lies primarily in the southern constellation [[Dorado]] and is one of the richest galaxy groups of the [[Southern Hemisphere]].<ref name="Laurikainenetal2006">{{citation |
|||
| url = http://adsabs.harvard.edu/abs/2006AJ....132.2634L |
|||
| title = The Near-infrared S0 Survey III: Morphology of 15 Southern Early-Type Disk Galaxies |
|||
| authors = Laurikainen, Eija; Salo, Heikki; Buta, Ronald; Knapen, Johan; Speltincx, Tom; Block, David |
|||
| year = 2006 |
|||
| date = December 2006 |
|||
| journal = The Astronomical Journal |
|||
| volume = 132 |
|||
| issue = 6 |
|||
| pages = 2634–2652 |
|||
| doi = 10.1086/508810 |
|||
}}</ref> [[Gérard de Vaucouleurs]] was the first to identify it in 1975 as a large complex nebulae II in the Dorado region,<ref name="Carrascoetal2001" /> designating it as G16.<ref name="Fergusonetal1990" /> |
|||
==Characteristics== |
==Characteristics== |
||
A rough distance estimate from NGC 1549 (using the [[Hubble constant]] as 70) |
A rough distance estimate from NGC 1549 (using the [[Hubble constant]] as 70) put the cluster at 18.4 [[Megaparsec|megaparsecs (Mpc)]].<ref name="Carrascoetal2001" /> The [[Cepheid variable|Cepheid]] distance estimate from Freedman et al. 2001 is 15.3 Mpc.<ref name="Evstigneevaetal2007">{{citation | bibcode = 2007MNRAS.378.1036E | title = Searches for ultracompact dwarf galaxies in galaxy groups | doi = 10.1111/j.1365-2966.2007.11856.x | date = July 2007 | journal = [[Monthly Notices of the Royal Astronomical Society]] | volume = 378 | issue = 3 | pages = 1036–1042 |
||
|author1=Evstigneeva, E. A. |author2=Drinkwater, M. J. |author3=Jurek, R. |author4=Firth, P. |author5=Jones, J. B. |author6=Gregg, M. D. |author7=Phillipps, S. |arxiv = 0704.1750 | s2cid = 15880069 }}</ref> Based upon the 2001 work of Tonry et al.<ref name="tonryetal2001">{{Citation |author1=J. L. Tonry |author2=A. Dressler |author3=J. P. Blakeslee |author4=E. A. Ajhar |author5=A. B. Fletcher |author6=G. A. Luppino |author7=M. R. Metzger |author8=C. B. Moore | title=The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances | journal=Astrophysical Journal | year=2001 | volume=546 | issue=2 | pages=681–693 | bibcode=2001ApJ...546..681T | doi=10.1086/318301 |arxiv = astro-ph/0011223 |s2cid=17628238 }}</ref> the [[surface brightness fluctuation]] (SBF) of six member galaxies was averaged and adjusted to estimate the group's distance at {{val|19.1|0.8|u=Mpc}} in 2007.<ref name="DeGraaffetal2007" /> |
|||
| url = http://adsabs.harvard.edu/abs/2007MNRAS.378.1036E |
|||
| title = Searches for ultracompact dwarf galaxies in galaxy groups |
|||
| doi = 10.1111/j.1365-2966.2007.11856.x |
|||
| authors = Evstigneeva, E. A.; Drinkwater, M. J.; Jurek, R.; Firth, P.; Jones, J. B.; Gregg, M. D.; Phillipps, S. |
|||
| year = 2007 |
|||
| date = July 2007 |
|||
| journal = Monthly Notices of the Royal Astronomical Society |
|||
| volume = 378 |
|||
| issue = 3 |
|||
| pages = 1036–1042 |
|||
}}</ref> Based upon the 2001 work of Tonry et al.<ref name="tonryetal2001">{{cite journal |
|||
| author=J. L. Tonry, A. Dressler, J. P. Blakeslee, E. A. Ajhar, A. B. Fletcher, G. A. Luppino, M. R. Metzger, C. B. Moore |
|||
| title=The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances |
|||
| journal=Astrophysical Journal |
|||
| year=2001 |
|||
| volume=546 |
|||
| issue=2 |
|||
| pages=681–693 |
|||
| url=http://adsabs.harvard.edu/abs/2001ApJ...546..681T |
|||
| doi=10.1086/318301 }}</ref> the [[surface brightness fluctuation]] (SBF) of six member galaxies was averaged and adjusted to estimate the group's distance at 19.1 ± 0.8 Mpc in 2007.<ref name="DeGraaffetal2007" /> |
|||
At the center of the cluster lie [[interacting galaxy|interacting galaxies]]<ref name="Bridgesetal1990">{{citation | bibcode = 1990AJ.....99.1100B | title = Globular clusters in the interacting galaxies NGC 1549 and NGC 1553 | date = April 1990 | journal = Astronomical Journal | issn = 0004-6256 | volume = 99 | pages = 1100–1107, 1340, 1341 | doi = 10.1086/115399 |author1=Bridges, Terry J. |author2=Hanes, David A. }}</ref> [[NGC 1549]] and [[NGC 1553]]. The dominant group members, ordered by luminosity, are: spiral [[NGC 1566]], [[lenticular galaxy|lenticular]] NGC 1553, and elliptical NGC 1549.<ref name="Firthetal2006">{{citation | bibcode = 2006MNRAS.372.1856F | date = November 2006 | title = Kinematics, substructure and luminosity-weighted dynamics of six nearby galaxy groups | journal = Monthly Notices of the Royal Astronomical Society | volume = 372 | issue = 4 | pages = 1856–1868 | doi = 10.1111/j.1365-2966.2006.10993.x |author1=Firth, P. |author2=Evstigneeva, E. A. |author3=Jones, J. B. |author4=Drinkwater, M. J. |author5=Phillipps, S. |author6=Gregg, M. D. |arxiv = astro-ph/0608584 | s2cid = 18646500 }}</ref> The group spans an area of the sky 10° square, corresponding to an actual area of around 3 Mpc square.<ref name="Carrascoetal2001" /> The group exhibits a relatively small [[harmonic mean]] radius (230 ± 40 kpc) due to the concentration at its core of more luminous galaxies.<ref name="Firthetal2006" /> All together, the group has an overall luminosity of 7.8 ± 1.6 {{e|10}} [[solar luminosity|''L''<sub>⊙</sub>]].<ref name="Firthetal2006" /> |
|||
At the center of the cluster lie [[interacting galaxy|interacting galaxies]]<ref name="Bridgesetal1990">{{citation |
|||
| url = http://adsabs.harvard.edu/abs/1990AJ.....99.1100B |
|||
| title = Globular clusters in the interacting galaxies NGC 1549 and NGC 1553 |
|||
| year = 1990 |
|||
| date = April 1990 |
|||
| journal = Astronomical Journal |
|||
| issn = 0004-6256 |
|||
| volume = 99 |
|||
| pages = 1100–1107, 1340, 1341 |
|||
| authors = Bridges, Terry J.; Hanes, David A. |
|||
| doi = 10.1086/115399 |
|||
}}</ref> NGC 1549 and [[NGC 1553]]. The dominant group members, ordered by luminosity, are: spiral [[NGC 1566]], [[lenticular galaxy|lenticular]] NGC 1553, and elliptical NGC 1549.<ref name="Firthetal2006">{{citation |
|||
| url = http://adsabs.harvard.edu/abs/2006MNRAS.372.1856F |
|||
| year = 2006 |
|||
| date = November 2006 |
|||
| title = Kinematics, substructure and luminosity-weighted dynamics of six nearby galaxy groups |
|||
| authors = Firth, P.; Evstigneeva, E. A.; Jones, J. B.; Drinkwater, M. J.; Phillipps, S.; Gregg, M. D. |
|||
| journal = Monthly Notices of the Royal Astronomical Society |
|||
| volume = 372 |
|||
| issue = 4 |
|||
| pages = 1856–1868 |
|||
| doi = 10.1111/j.1365-2966.2006.10993.x |
|||
}}</ref> The group spans an area of the sky 10° square which represents around 3 Mpc square.<ref name="Carrascoetal2001" /> The group exhibits a relatively small [[harmonic mean]] radius (230 ± 40 kpc) due to the concentration at its core of more luminous galaxies.<ref name="Firthetal2006" /> All together, the group has an overall luminosity of 7.8 ± 1.6 {{e|10}} [[solar luminosity|''L''<sub>⊙</sub>]].<ref name="Firthetal2006" /> |
|||
The Dorado Group contains three dominant smaller groups within itself, NGC 1672 Group, NGC 1566 Group and the NGC 1433 Group, as evidenced by the [[H I region|H I]] distribution of the region.<ref name="Kilbornetal2005" /> The Dorado Group is in the Fornax Wall that connects these three groups.<ref name="Kilbornetal2005">{{citation |
The Dorado Group contains three dominant smaller groups within itself, [[NGC 1672 Group]], [[NGC 1566 Group]] and the [[NGC 1433 Group]], as evidenced by the [[H I region|H I]] distribution of the region.<ref name="Kilbornetal2005" /> The Dorado Group is in the [[Fornax Wall]] that connects these three groups.<ref name="Kilbornetal2005">{{citation | bibcode = 2005MNRAS.356...77K | title = A Wide-Field Hi Study of the NGC 1566 Group | date = January 2005 | journal = Monthly Notices of the Royal Astronomical Society | volume = 356 | issue = 1 | pages = 77–88 | doi = 10.1111/j.1365-2966.2004.08450.x |author1= Virginia A. Kilborn |author2=[[Bärbel Koribalski|Bärbel S. Koribalski]] |author3=Duncan A. Forbes |author4=David G. Barnes |author5=Ruth C. Musgrave |
||
|arxiv = astro-ph/0409743 }}</ref> Due to its location in the Fornax Wall, the group is at a similar distance as the [[Fornax Cluster]].<ref name="DeGraaffetal2007">{{Citation |author1=DeGraaff, Regina Barber |author2=Blakeslee, John P. |author3=Meurer, Gerhardt R. |author4=Putman, Mary E. | title = A Galaxy in Transition: Structure, Globular Clusters, and Distance of the Star-Forming S0 Galaxy NGC 1533 in Dorado | journal = The Astrophysical Journal | date = December 2007 | volume = 671 | issue = 2 | pages = 1624–1639 | bibcode = 2007ApJ...671.1624D | doi = 10.1086/523640 |
|||
| url = http://adsabs.harvard.edu/abs/2005MNRAS.356...77K |
|||
|arxiv=0710.0893|s2cid=14312626 }}</ref> The Dorado Group is richer than the [[Local Group]], while still being dominated by disk [[Galaxy morphological classification|types of galaxies]] (i.e. its two brightest members are spiral NGC 1566 and lenticular NGC 1553) and its member galaxies have H I masses on par with [[interacting galaxy|non-interacting galaxies]] of the same morphological type.<ref name="DeGraaffetal2007" /> With the group's apparent crossing time being 12.6 ± 0.6 %<ref name="Firthetal2006" /> of the [[age of the universe|universe's age]], recent analyses deduce that the group is [[Virial theorem|unvirialized]], and thus this may explain the abundance of spirals and H I.<ref name="DeGraaffetal2007" /> |
|||
| title = A Wide-Field Hi Study of the NGC 1566 Group |
|||
| year = 2005 |
|||
| date = January 2005 |
|||
| journal = Monthly Notices of the Royal Astronomical Society |
|||
| volume = 356 |
|||
| issue = 1 |
|||
| pages = 77–88 |
|||
| authors = Virginia A. Kilborn; Bärbel S. Koribalski; Duncan A. Forbes; David G. Barnes; Ruth C. Musgrave |
|||
| doi = 10.1111/j.1365-2966.2004.08450.x |
|||
}}</ref> Because it is in the Fornax Wall, it is at a similar distance as the [[Fornax Cluster]].<ref name="DeGraaffetal2007">{{cite journal |
|||
| author = DeGraaff, Regina Barber; Blakeslee, John P.; Meurer, Gerhardt R.; Putman, Mary E. |
|||
| title = A Galaxy in Transition: Structure, Globular Clusters, and Distance of the Star-Forming S0 Galaxy NGC 1533 in Dorado |
|||
| journal = The Astrophysical Journal |
|||
| year = 2007 |
|||
| date = December 2007 |
|||
| volume = 671 |
|||
| issue = 2 |
|||
| pages = 1624–1639 |
|||
| url = http://adsabs.harvard.edu/abs/2007ApJ...671.1624D |
|||
| doi = 10.1086/523640 |
|||
}}</ref> The Dorado Group is interesting for being richer than the [[Local Group]], while still being dominated by disk [[Galaxy morphological classification|types of galaxies]] (i.e. its two brightest members are spiral NGC 1566 and lenticular NGC 1553) and its member galaxies have H I masses on par with [[interacting galaxy|non-interacting galaxies]] of the same morphological type.<ref name="DeGraaffetal2007" /> With the group's apparent crossing time being 12.6 ± 0.6<ref name="Firthetal2006" /> % of the [[age of the universe|universe's age]], recent analyses deduce that the group is [[Virial theorem|unvirialized]], and thus this may explain the abundance of spirals and H I.<ref name="DeGraaffetal2007" /> |
|||
==Members== |
==Members== |
||
The table below lists eighteen galaxies that were identified in 1982 as associated with the Dorado Group by [[John Peter Huchra]] and [[Margaret J. Geller]] with the ones later dropped struck out.<ref name="Huchraetal1982">{{citation | bibcode = 1982ApJ...257..423H | title = Groups of galaxies. I – Nearby groups | last1 = Huchra | first1 = John Peter | author-link1 = John Peter Huchra | last2 = Geller | first2 = Margaret J. | author-link2 = Margaret J. Geller | doi = 10.1086/160000 | date = June 15, 1982 | journal = Astrophysical Journal | issue = Part 1 | volume = 257 | pages = 423–437}}</ref> In 1989, the list of members was expanded to 46 by Maia, da Costa, & Latham.<ref name="Carrascoetal2001" /> In 1990–1991, Henry C. Ferguson and [[Allan Sandage]] identified 34 other possible candidate members of the group with magnitudes greater than 19 and eliminated one member from Maia et al. putting the list at 79<ref name="Firthetal2006" /> galaxies.<ref name="Carrascoetal2001" /><ref name="Fergusonetal1990" /> Kilborn et al. 2005 confirmed 26 members from the list.<ref name="Kilbornetal2005" /> In 2006, the list was refined again by Firth et al.<ref name="Firthetal2006" /> Using [[redshift]] data, they excluded eleven (as being background galaxies or interloper) from the Ferguson et al. list, confirmed the membership of twenty on the list, and left 48 unconfirmed.<ref name="Firthetal2006" /> |
|||
The table below lists eighteen galaxies that were identified in 1982 as associated with the Dorado Group by [[John Peter Huchra]] and [[Margaret J. Geller]] with the ones later dropped stuck out.<ref name="Huchraetal1982">{{citation |
|||
| url = http://adsabs.harvard.edu/abs/1982ApJ...257..423H |
|||
| title = Groups of galaxies. I - Nearby groups |
|||
| last1 = Huchra |
|||
| first1 = John Peter |
|||
| authorlink1 = John Peter Huchra |
|||
| last2 = Geller |
|||
| first2 = Margaret J. |
|||
| authorlink2 = Margaret J. Geller |
|||
| doi = 10.1086/160000 |
|||
| year = 1982 |
|||
| date = [[June 15]] [[1982]] |
|||
| journal = Astrophysical Journal |
|||
| issue = Part 1 |
|||
| volume = 257 |
|||
| pages = 423–437 |
|||
}}</ref> In 1989, the list of members was expanded to 46 by Maia, da Costa, & Latham.<ref name="Carrascoetal2001" /> Lastly, in 1990/1991, Henry C. Ferguson & [[Allan Sandage]] identified 34 other possible candidate members of the group with magnitudes greater than 19 and eliminated one member from Maia et al. putting the list at 79<ref name="Firthetal2006" /> galaxies.<ref name="Fergusonetal1990" /><ref name="Carrascoetal2001" /> Kilborn et al. 2005 confirmed 26 members from the list.<ref name="Kilbornetal2005" /> In 2006, the list was refined again by Firth et al.<ref name="Firthetal2006" /> Using [[redshift]] data, they excluded eleven (as being background galaxies or interloper) from the Ferguson et al. list, confirmed the membership of twenty on the list, and left 48 unconfirmed.<ref name="Firthetal2006" /> |
|||
{{clear}} |
|||
{| class="wikitable" style="text-align:center;border-collapse:collapse;" cellpadding="2" |
{| class="wikitable" style="text-align:center;border-collapse:collapse;" cellpadding="2" |
||
|+'''Huchra et al. 1982 Members of the Dorado Group<br>(with |
|+'''Huchra et al. 1982 Members of the Dorado Group<br>(with strikeouts for ones dropped by Maia et al. in 1989)''' |
||
|- |
|- |
||
! style="background:#efefef;" | Name |
! style="background:#efefef;" | Name |
||
Line 152: | Line 48: | ||
! style="background:#efefef;" | [[Right Ascension|R.A.]] ([[J2000]])<ref name="ned" /> |
! style="background:#efefef;" | [[Right Ascension|R.A.]] ([[J2000]])<ref name="ned" /> |
||
! style="background:#efefef;" | [[Declination|Dec.]] ([[J2000]])<ref name="ned" /> |
! style="background:#efefef;" | [[Declination|Dec.]] ([[J2000]])<ref name="ned" /> |
||
! style="background:#efefef;" | [[Redshift]] ( |
! style="background:#efefef;" | [[Redshift]] (km/[[second|s]])<ref name="ned" /> |
||
! style="background:#efefef;" | [[Apparent Magnitude]]<ref name="ned" /> |
! style="background:#efefef;" | [[Apparent Magnitude]]<ref name="ned" /> |
||
|- |
|- |
||
Line 161: | Line 57: | ||
| 1184 ± 6 |
| 1184 ± 6 |
||
| 12.6 |
| 12.6 |
||
|- |
|- |
||
| <s>[[NGC 1947]]</s> |
| <s>[[NGC 1947]]</s> |
||
| S0<sup> |
| S0<sup>−</sup> pec |
||
| {{RA|05|26|47.6}} |
| {{RA|05|26|47.6}} |
||
| {{DEC|-63|45|36}} |
| {{DEC|-63|45|36}} |
||
| 1100 ± 24 |
| 1100 ± 24 |
||
| 11.7 |
| 11.7 |
||
|- |
|- |
||
| <s>[[NGC 1796]]</s> |
| <s>[[NGC 1796]]</s> |
||
| (R)SB(r)dm: |
| (R)SB(r)dm: |
||
Line 175: | Line 71: | ||
| 1014 ± 9 |
| 1014 ± 9 |
||
| 12.9 |
| 12.9 |
||
|- |
|- |
||
| <s>[[NGC 1688]]</s> |
| <s>[[NGC 1688]]</s> |
||
| SB(rs)dm |
| SB(rs)dm |
||
Line 182: | Line 78: | ||
| 1228 ± 6 |
| 1228 ± 6 |
||
| 12.6 |
| 12.6 |
||
|- |
|- |
||
| <s>[[NGC 1672]]</s> |
| <s>[[NGC 1672]]</s> |
||
| (R'_1:)SB(r)bc Sy2 |
| (R'_1:)SB(r)bc Sy2 |
||
Line 189: | Line 85: | ||
| 1331 ± 3 |
| 1331 ± 3 |
||
| 10.3 |
| 10.3 |
||
|- |
|- |
||
| [[IC 2056]] |
| [[IC 2056]] |
||
| SAB(r)b |
| SAB(r)b |
||
Line 196: | Line 92: | ||
| 1133 ± 10 |
| 1133 ± 10 |
||
| 12.5 |
| 12.5 |
||
|- |
|- |
||
| <s>[[NGC 1559]]</s> |
| <s>[[NGC 1559]]</s> |
||
| SB(s)cd |
| SB(s)cd |
||
Line 203: | Line 99: | ||
| 1304 ± 4 |
| 1304 ± 4 |
||
| 11.0 |
| 11.0 |
||
|- |
|- |
||
| [[NGC 1543]] |
| [[NGC 1543]] |
||
| (R)SB(l)0<sup>0</sup> |
| (R)SB(l)0<sup>0</sup> |
||
Line 210: | Line 106: | ||
| 1176 ± 7 |
| 1176 ± 7 |
||
| 11.5 |
| 11.5 |
||
|- |
|- |
||
| [[NGC 1574]] |
| [[NGC 1574]] |
||
| SA0<sup> |
| SA0<sup>−</sup> |
||
| {{RA|04|21|58.8}} |
| {{RA|04|21|58.8}} |
||
| {{DEC|-56|58|29}} |
| {{DEC|-56|58|29}} |
||
| 1050 ± 25 |
| 1050 ± 25 |
||
| 11.4 |
| 11.4 |
||
|- |
|- |
||
| [[NGC 1533]] |
| [[NGC 1533]] |
||
| (L)SB(rs)0<sup>0</sup> |
| (L)SB(rs)0<sup>0</sup> |
||
Line 224: | Line 120: | ||
| 790 ± 5 |
| 790 ± 5 |
||
| 11.7 |
| 11.7 |
||
|- |
|- |
||
| [[NGC 1546]] |
| [[NGC 1546]] |
||
| SA0<sup>+?</sup> |
| SA0<sup>+?</sup> |
||
Line 231: | Line 127: | ||
| 1284 ± 14 |
| 1284 ± 14 |
||
| 11.8 |
| 11.8 |
||
|- |
|- |
||
| [[NGC 1553]] |
| [[NGC 1553]] |
||
| SA(rl)0<sup>0</sup> |
| SA(rl)0<sup>0</sup> |
||
Line 238: | Line 134: | ||
| 1080 ± 11 |
| 1080 ± 11 |
||
| 10.3 |
| 10.3 |
||
|- |
|- |
||
| [[NGC 1549]] |
| [[NGC 1549]] |
||
| E0<sup> |
| E0<sup>−1</sup> |
||
| {{RA|04|15|45.1}} |
| {{RA|04|15|45.1}} |
||
| {{DEC|-55|35|32}} |
| {{DEC|-55|35|32}} |
||
| 1220 ± 15 |
| 1220 ± 15 |
||
| 10.7 |
| 10.7 |
||
|- |
|- |
||
| [[NGC 1566]] |
| [[NGC 1566]] |
||
| (R'_1)SAB(rs)bcSy1 |
| (R'_1)SAB(rs)bcSy1 |
||
Line 252: | Line 148: | ||
| 1504 ± 2 |
| 1504 ± 2 |
||
| 10.3 |
| 10.3 |
||
|- |
|- |
||
| [[NGC 1617]] |
| [[NGC 1617]] |
||
| (R')SAB(rs)a |
| (R')SAB(rs)a |
||
Line 259: | Line 155: | ||
| 1063 ± 21 |
| 1063 ± 21 |
||
| 11.4 |
| 11.4 |
||
|- |
|- |
||
| [[NGC 1515]] |
| [[NGC 1515]] |
||
| SAB(s)bc |
| SAB(s)bc |
||
Line 266: | Line 162: | ||
| 1175 ± 7 |
| 1175 ± 7 |
||
| 12.1 |
| 12.1 |
||
|- |
|- |
||
| [[NGC 1705]] |
| [[NGC 1705]] |
||
| SA0<sup> |
| SA0<sup>−</sup> pec |
||
| {{RA|04|54|13.5}} |
| {{RA|04|54|13.5}} |
||
| {{DEC|-53|21|40}} |
| {{DEC|-53|21|40}} |
||
| 633 ± 6 |
| 633 ± 6 |
||
| 12.8 |
| 12.8 |
||
|- |
|- |
||
| [[NGC 1596]] |
| [[NGC 1596]] |
||
| SA0: sp |
| SA0: sp |
||
Line 280: | Line 176: | ||
| 1510 ± 8 |
| 1510 ± 8 |
||
| 12.1 |
| 12.1 |
||
|- |
|- |
||
|} |
|} |
||
[[File:NGC 1487 HST.jpg|thumb|Peculiar galaxy [[NGC 1487]] is located about 30 million light-years away in the constellation of [[Eridanus (constellation)|Eridanus]].<ref>{{cite web|title=One from many|url=http://www.spacetelescope.org/images/potw1605a/|access-date=1 February 2016}}</ref>]] |
|||
The Maia et al. 1989 thirty-four added members were: [[IC 2049]], [[NGC 1536]], [[IC 2058]], [[IC 2032]], [[NGC 1602]], [[NGC 1581]], [[IC 2085]], [[NGC 1522]], [[PGC 15149]], [[NGC 1556]], [[NGC 1527]], [[NGC 1494]], [[NGC 1493]], [[PGC 14416]], [[IC 2000]], [[NGC 1483]], [[NGC 1433]], [[PGC 14078]] , [[NGC 1495]], [[NGC 1510]], [[NGC 1512]], [[IC 1959]], [[IC 1986]], [[NGC 1448]], [[NGC 1487]], [[IC 1933]], [[NGC 1311]], [[IC 1954]], [[IC 1914]], [[NGC 1411]], [[IC 1970]], [[PGC 13818]], [[NGC 1249]], and [[PGC 11139]].<ref name="Maiaetal1989">{{citation |
|||
| url = http://adsabs.harvard.edu/abs/1989ApJS...69..809M |
|||
| authors = Maia, M. A. G.; da Costa, L. N.; Latham, David W. |
|||
| year = 1989 |
|||
| date = April 1989 |
|||
| journal = Astrophysical Journal Supplement Series |
|||
| issn = 0067-0049 |
|||
| volume = 69 |
|||
| pages = 809–829 |
|||
| doi = 10.1086/191328 |
|||
| title = A catalog of southern groups of galaxies |
|||
}}</ref> And the six dropped from the 1982 list were: [[NGC 2082]], [[NGC 1947]], [[NGC 1796]], [[NGC 1688]], [[NGC 1672]], and [[NGC 1559]].<ref name="Maiaetal1989" /> In 2007, a study of [[ultracompact dwarf]]s (UCD) identified one definite and two possible UCD members of the group.<ref name="Evstigneevaetal2007" /> The thirty-four added by Ferguson et al. 1990 included [[IC 2038]] and [[IC 2039]].<ref name="Fergusonetal1990" /> |
|||
The Maia et al. 1989 thirty-four added members were: [[IC 2049]], [[NGC 1536]], [[IC 2058]], [[IC 2032]], [[NGC 1602]], [[NGC 1581]], [[IC 2085]], [[NGC 1522]], [[PGC 15149]], [[NGC 1556]], [[NGC 1527]], [[NGC 1494]], [[NGC 1493]], [[PGC 14416]], IC 2000, [[NGC 1483]], [[NGC 1433]], [[PGC 14078]], [[NGC 1495]], [[NGC 1510]], [[NGC 1510]], [[NGC 1512]], [[IC 1959]], [[IC 1986]], [[NGC 1448]], [[NGC 1487]], [[IC 1933]], [[NGC 1311]], [[IC 1954]], [[IC 1914]], [[NGC 1411]], [[IC 1970]], [[PGC 13818]], [[NGC 1249]], and [[PGC 11139]].<ref name="Maiaetal1989">{{citation | bibcode = 1989ApJS...69..809M | date = April 1989 | journal = Astrophysical Journal Supplement Series | issn = 0067-0049 | volume = 69 | pages = 809–829 | doi = 10.1086/191328 | title = A catalog of southern groups of galaxies |author1=Maia, M. A. G. |author2=da Costa, L. N. |author3=Latham, David W. | doi-access = free }}</ref> And the six dropped from the 1982 list were: [[NGC 2082]], [[NGC 1947]], [[NGC 1796]], [[NGC 1688]], [[NGC 1672]], and [[NGC 1559]].<ref name="Maiaetal1989" /> In 2007, a study of [[ultracompact dwarf]]s (UCD) identified one definite and two possible UCD members of the group.<ref name="Evstigneevaetal2007" /> The thirty-four added by Ferguson et al. 1990 included [[IC 2038]] and [[IC 2039]].<ref name="Fergusonetal1990" /> |
|||
The NGC 1566 Group of Dorado contains [[H I region|H I]] with ''M''<sub>HI</sub> = 3.5{{e|10}} ''M''<sub>⊙</sub> of which 40% alone comes from the NGC 1566 galaxy.<ref name="Kilbornetal2005" /> More than half of its members are outside its virial radius of 580 kpc which suggests this group is a young non-virialized group. The 2005 Kilborn et al. set of confirmed NGC 1566 Group members (within the Dorado Group) is:<ref name="Kilbornetal2005" /> |
|||
The NGC 1566 Group of Dorado contains [[H I region|H I]] with ''M''<sub>HI</sub> = 3.5{{e|10}} ''M''<sub>⊙</sub> of which 40% alone comes from the NGC 1566 galaxy.<ref name="Kilbornetal2005" /> More than half of its members are outside its virial radius of 580 kpc which suggests this group is a young non-virialized group. The 2005 Kilborn et al. set of confirmed NGC 1566 Group members (within the Dorado Group) is:<ref name="Kilbornetal2005" /> |
|||
{{clear}} |
{{clear}} |
||
{| class="wikitable" style="text-align:center;border-collapse:collapse;" cellpadding="2" |
{| class="wikitable" style="text-align:center;border-collapse:collapse;" cellpadding="2" |
||
Line 305: | Line 192: | ||
! style="background:#efefef;" | [[Right Ascension|R.A.]] ([[J2000]])<ref name="ned" /> |
! style="background:#efefef;" | [[Right Ascension|R.A.]] ([[J2000]])<ref name="ned" /> |
||
! style="background:#efefef;" | [[Declination|Dec.]] ([[J2000]])<ref name="ned" /> |
! style="background:#efefef;" | [[Declination|Dec.]] ([[J2000]])<ref name="ned" /> |
||
! style="background:#efefef;" | [[Redshift]] ( |
! style="background:#efefef;" | [[Redshift]] (km/[[second|s]])<ref name="ned" /> |
||
! style="background:#efefef;" | [[Apparent Magnitude]]<ref name="ned" /> |
! style="background:#efefef;" | [[Apparent Magnitude]]<ref name="ned" /> |
||
|- |
|- |
||
| [[IC 2049]] |
| [[IC 2049]] |
||
| SAB(s)d? |
| SAB(s)d? |
||
Line 314: | Line 201: | ||
| 1469 ± 7 |
| 1469 ± 7 |
||
| 14.5 |
| 14.5 |
||
|- |
|- |
||
| [[NGC 1536]] |
| [[NGC 1536]] |
||
| SB(s)c pec |
| SB(s)c pec |
||
Line 321: | Line 208: | ||
| 1217 ± 13 |
| 1217 ± 13 |
||
| 13.2 |
| 13.2 |
||
|- |
|- |
||
| [[NGC 1543]] |
| [[NGC 1543]] |
||
| (R)SB(l)0<sup>0</sup> |
| (R)SB(l)0<sup>0</sup> |
||
Line 328: | Line 215: | ||
| 1176 ± 7 |
| 1176 ± 7 |
||
| 11.5 |
| 11.5 |
||
|- |
|- |
||
| [[LSBG F157-081]] |
| [[LSBG F157-081]] |
||
| Irregular |
| Irregular |
||
Line 335: | Line 222: | ||
| 1215 ± 7 |
| 1215 ± 7 |
||
| 16.7 |
| 16.7 |
||
|- |
|- |
||
| [[NGC 1533]] |
| [[NGC 1533]] |
||
| (L)SB(rs)0<sup>0</sup> |
| (L)SB(rs)0<sup>0</sup> |
||
Line 342: | Line 229: | ||
| 790 ± 5 |
| 790 ± 5 |
||
| 11.7 |
| 11.7 |
||
|- |
|- |
||
| [[IC 2038]] |
| [[IC 2038]] |
||
| Sd pec |
| Sd pec |
||
Line 349: | Line 236: | ||
| 712 ± 52 |
| 712 ± 52 |
||
| 15.5 |
| 15.5 |
||
|- |
|- |
||
| [[APMBGC 157+016+068]] |
| [[APMBGC 157+016+068]] |
||
| Irregular |
| Irregular |
||
Line 356: | Line 243: | ||
| 1350 ± 4 |
| 1350 ± 4 |
||
| 16.3 |
| 16.3 |
||
|- |
|- |
||
| [[NGC 1546]] |
| [[NGC 1546]] |
||
| SA0<sup>+?</sup> |
| SA0<sup>+?</sup> |
||
Line 363: | Line 250: | ||
| 1284 ± 14 |
| 1284 ± 14 |
||
| 11.8 |
| 11.8 |
||
|- |
|- |
||
| [[IC 2058]] |
| [[IC 2058]] |
||
| Sc |
| Sc |
||
Line 370: | Line 257: | ||
| 1379 ± 1 |
| 1379 ± 1 |
||
| 13.9 |
| 13.9 |
||
|- |
|- |
||
| [[IC 2032]] |
| [[IC 2032]] |
||
| IAB(s)m pec |
| IAB(s)m pec |
||
Line 377: | Line 264: | ||
| 1068 ± 7 |
| 1068 ± 7 |
||
| 14.7 |
| 14.7 |
||
|- |
|- |
||
| [[NGC 1566]] |
| [[NGC 1566]] |
||
| (R'_1)SAB(rs)bcSy1 |
| (R'_1)SAB(rs)bcSy1 |
||
Line 384: | Line 271: | ||
| 1504 ± 2 |
| 1504 ± 2 |
||
| 10.3 |
| 10.3 |
||
|- |
|- |
||
| [[NGC 1596]] |
| [[NGC 1596]] |
||
| SA0: sp |
| SA0: sp |
||
Line 391: | Line 278: | ||
| 1510 ± 8 |
| 1510 ± 8 |
||
| 12.1 |
| 12.1 |
||
|- |
|- |
||
| [[NGC 1602]] |
| [[NGC 1602]] |
||
| IB(s)m pec |
| IB(s)m pec |
||
Line 398: | Line 285: | ||
| 1568 ± 8 |
| 1568 ± 8 |
||
| 13.3 |
| 13.3 |
||
|- |
|- |
||
| [[NGC 1515]] |
| [[NGC 1515]] |
||
| SAB(s)bc |
| SAB(s)bc |
||
Line 405: | Line 292: | ||
| 1175 ± 7 |
| 1175 ± 7 |
||
| 12.1 |
| 12.1 |
||
|- |
|- |
||
| [[NGC 1522]] |
| [[NGC 1522]] |
||
| (R')S0<sup>0</sup>: pec |
| (R')S0<sup>0</sup>: pec |
||
Line 412: | Line 299: | ||
| 898 ± 7 |
| 898 ± 7 |
||
| 13.9 |
| 13.9 |
||
|- |
|- |
||
| [[ESO 118-019]] |
| [[ESO 118-019]] |
||
| S0<sup>0</sup> pec |
| S0<sup>0</sup> pec |
||
| {{RA|04|18|59.5}} |
| {{RA|04|18|59.5}} |
||
| {{DEC|-58|15|27}} |
| {{DEC|-58|15|27}} |
||
| 1239 |
| 1239 |
||
| 14.9 |
| 14.9 |
||
|- |
|- |
||
| [[ESO 157-030]] |
| [[ESO 157-030]] |
||
| E4 |
| E4 |
||
Line 426: | Line 313: | ||
| 1471 ± 28 |
| 1471 ± 28 |
||
| 14.7 |
| 14.7 |
||
|- |
|- |
||
| [[ESO 157-047]] |
| [[ESO 157-047]] |
||
| S0/a? pec sp |
| S0/a? pec sp |
||
Line 433: | Line 320: | ||
| 1655 ± 10 |
| 1655 ± 10 |
||
| 15.5 |
| 15.5 |
||
|- |
|- |
||
| [[ESO 157-049]] |
| [[ESO 157-049]] |
||
| S? |
| S? |
||
Line 440: | Line 327: | ||
| 1678 ± 5 |
| 1678 ± 5 |
||
| 14.3 |
| 14.3 |
||
|- |
|- |
||
| [[IC 2085]] |
| [[IC 2085]] |
||
| S0<sup>0</sup> pec sp |
| S0<sup>0</sup> pec sp |
||
Line 447: | Line 334: | ||
| 982 ± 10 |
| 982 ± 10 |
||
| 13.9 |
| 13.9 |
||
|- |
|- |
||
| [[NGC 1549]] |
| [[NGC 1549]] |
||
| E0<sup> |
| E0<sup>−1</sup> |
||
| {{RA|04|15|45.1}} |
| {{RA|04|15|45.1}} |
||
| {{DEC|-55|35|32}} |
| {{DEC|-55|35|32}} |
||
| 1220 ± 15 |
| 1220 ± 15 |
||
| 10.7 |
| 10.7 |
||
|- |
|- |
||
| [[NGC 1553]] |
| [[NGC 1553]] |
||
| SA(rl)0<sup>0</sup> |
| SA(rl)0<sup>0</sup> |
||
Line 461: | Line 348: | ||
| 1080 ± 11 |
| 1080 ± 11 |
||
| 10.3 |
| 10.3 |
||
|- |
|- |
||
| [[NGC 1574]] |
| [[NGC 1574]] |
||
| SA0<sup> |
| SA0<sup>−</sup> |
||
| {{RA|04|21|58.8}} |
| {{RA|04|21|58.8}} |
||
| {{DEC|-56|58|29}} |
| {{DEC|-56|58|29}} |
||
| 1050 ± 25 |
| 1050 ± 25 |
||
| 11.4 |
| 11.4 |
||
|- |
|- |
||
| [[NGC 1581]] |
| [[NGC 1581]] |
||
| S0<sup> |
| S0<sup>−</sup> |
||
| {{RA|04|24|44.9}} |
| {{RA|04|24|44.9}} |
||
| {{DEC|-54|56|31}} |
| {{DEC|-54|56|31}} |
||
| 1600 ± 27 |
| 1600 ± 27 |
||
| 13.6 |
| 13.6 |
||
|- |
|- |
||
| [[NGC 1617]] |
| [[NGC 1617]] |
||
| (R')SAB(rs)a |
| (R')SAB(rs)a |
||
Line 482: | Line 369: | ||
| 1063 ± 21 |
| 1063 ± 21 |
||
| 11.4 |
| 11.4 |
||
|- |
|- |
||
| [[Abell 3202]] |
| [[Abell 3202]] |
||
| Irregular |
| Irregular |
||
Line 489: | Line 376: | ||
| 1135 ± 40 |
| 1135 ± 40 |
||
| 16.9 |
| 16.9 |
||
|- |
|- |
||
|} |
|} |
||
Line 496: | Line 383: | ||
==References== |
==References== |
||
{{ |
{{Reflist}} |
||
{{Stars of Dorado}} |
|||
[[Category:Dorado Group| ]] |
|||
[[Category:Dorado constellation]] |
|||
{{Authority control}} |
|||
[[zh:劍魚座星系團]] |
|||
{{Sky|04|17|03.9|-|56|07|43|60000000}} |
|||
{{DEFAULTSORT:Dorado Group}} |
|||
[[Category:Dorado Group| ]] |
|||
[[Category:Dorado]] |
|||
[[Category:Southern Supercluster]] |
Revision as of 13:11, 12 August 2023
Dorado Group | |
---|---|
NGC 1566, one of the brightest members of the Dorado Group (Spitzer Space Telescope image) | |
Observation data (Epoch J2000) | |
Constellation(s) | Dorado |
Right ascension | 04h 17m 03.9s[1] |
Declination | −56° 07′ 43″[1] |
Brightest member | NGC 1566 |
Number of galaxies | 46 plus 34 candidate members[2] |
Other designations | |
Shk 18,[2] G16,[2][3] HG3,[2] MC13,[4] and NGC 1566 Group[5] |
The Dorado Group is a loose concentration of galaxies[2] containing both spirals and ellipticals.[3] It is generally considered a 'galaxy group' but may approach the size of a 'galaxy cluster'.[6] It lies primarily in the southern constellation Dorado and is one of the richest galaxy groups of the Southern Hemisphere.[7] Gérard de Vaucouleurs was the first to identify it in 1975 as a large complex nebulae II in the Dorado region,[2] designating it as G16.[3]
Characteristics
A rough distance estimate from NGC 1549 (using the Hubble constant as 70) put the cluster at 18.4 megaparsecs (Mpc).[2] The Cepheid distance estimate from Freedman et al. 2001 is 15.3 Mpc.[8] Based upon the 2001 work of Tonry et al.[9] the surface brightness fluctuation (SBF) of six member galaxies was averaged and adjusted to estimate the group's distance at 19.1±0.8 Mpc in 2007.[10]
At the center of the cluster lie interacting galaxies[11] NGC 1549 and NGC 1553. The dominant group members, ordered by luminosity, are: spiral NGC 1566, lenticular NGC 1553, and elliptical NGC 1549.[6] The group spans an area of the sky 10° square, corresponding to an actual area of around 3 Mpc square.[2] The group exhibits a relatively small harmonic mean radius (230 ± 40 kpc) due to the concentration at its core of more luminous galaxies.[6] All together, the group has an overall luminosity of 7.8 ± 1.6 ×1010 L⊙.[6]
The Dorado Group contains three dominant smaller groups within itself, NGC 1672 Group, NGC 1566 Group and the NGC 1433 Group, as evidenced by the H I distribution of the region.[5] The Dorado Group is in the Fornax Wall that connects these three groups.[5] Due to its location in the Fornax Wall, the group is at a similar distance as the Fornax Cluster.[10] The Dorado Group is richer than the Local Group, while still being dominated by disk types of galaxies (i.e. its two brightest members are spiral NGC 1566 and lenticular NGC 1553) and its member galaxies have H I masses on par with non-interacting galaxies of the same morphological type.[10] With the group's apparent crossing time being 12.6 ± 0.6 %[6] of the universe's age, recent analyses deduce that the group is unvirialized, and thus this may explain the abundance of spirals and H I.[10]
Members
The table below lists eighteen galaxies that were identified in 1982 as associated with the Dorado Group by John Peter Huchra and Margaret J. Geller with the ones later dropped struck out.[12] In 1989, the list of members was expanded to 46 by Maia, da Costa, & Latham.[2] In 1990–1991, Henry C. Ferguson and Allan Sandage identified 34 other possible candidate members of the group with magnitudes greater than 19 and eliminated one member from Maia et al. putting the list at 79[6] galaxies.[2][3] Kilborn et al. 2005 confirmed 26 members from the list.[5] In 2006, the list was refined again by Firth et al.[6] Using redshift data, they excluded eleven (as being background galaxies or interloper) from the Ferguson et al. list, confirmed the membership of twenty on the list, and left 48 unconfirmed.[6]
Name | Type[1] | R.A. (J2000)[1] | Dec. (J2000)[1] | Redshift (km/s)[1] | Apparent Magnitude[1] |
---|---|---|---|---|---|
SAB(rs+)c | 05h 41m 51.1s | −64° 18′ 04″ | 1184 ± 6 | 12.6 | |
S0− pec | 05h 26m 47.6s | −63° 45′ 36″ | 1100 ± 24 | 11.7 | |
(R)SB(r)dm: | 05h 02m 42.5s | −61° 08′ 24″ | 1014 ± 9 | 12.9 | |
SB(rs)dm | 04h 48m 23.8s | −59° 48′ 01″ | 1228 ± 6 | 12.6 | |
(R'_1:)SB(r)bc Sy2 | 04h 45m 42.5s | −59° 14′ 50″ | 1331 ± 3 | 10.3 | |
IC 2056 | SAB(r)b | 04h 16m 24.5s | −60° 12′ 25″ | 1133 ± 10 | 12.5 |
SB(s)cd | 04h 17m 35.8s | −62° 47′ 01″ | 1304 ± 4 | 11.0 | |
NGC 1543 | (R)SB(l)00 | 04h 12m 43.2s | −57° 44′ 17″ | 1176 ± 7 | 11.5 |
NGC 1574 | SA0− | 04h 21m 58.8s | −56° 58′ 29″ | 1050 ± 25 | 11.4 |
NGC 1533 | (L)SB(rs)00 | 04h 09m 51.8s | −56° 07′ 06″ | 790 ± 5 | 11.7 |
NGC 1546 | SA0+? | 04h 14m 36.5s | −56° 03′ 39″ | 1284 ± 14 | 11.8 |
NGC 1553 | SA(rl)00 | 04h 16m 10.5s | −55° 46′ 49″ | 1080 ± 11 | 10.3 |
NGC 1549 | E0−1 | 04h 15m 45.1s | −55° 35′ 32″ | 1220 ± 15 | 10.7 |
NGC 1566 | (R'_1)SAB(rs)bcSy1 | 04h 20m 00.4s | −54° 56′ 16″ | 1504 ± 2 | 10.3 |
NGC 1617 | (R')SAB(rs)a | 04h 31m 39.5s | −54° 36′ 08″ | 1063 ± 21 | 11.4 |
NGC 1515 | SAB(s)bc | 04h 04m 02.7s | −54° 06′ 00″ | 1175 ± 7 | 12.1 |
NGC 1705 | SA0− pec | 04h 54m 13.5s | −53° 21′ 40″ | 633 ± 6 | 12.8 |
NGC 1596 | SA0: sp | 04h 27m 38.1s | −55° 01′ 40″ | 1510 ± 8 | 12.1 |
The Maia et al. 1989 thirty-four added members were: IC 2049, NGC 1536, IC 2058, IC 2032, NGC 1602, NGC 1581, IC 2085, NGC 1522, PGC 15149, NGC 1556, NGC 1527, NGC 1494, NGC 1493, PGC 14416, IC 2000, NGC 1483, NGC 1433, PGC 14078, NGC 1495, NGC 1510, NGC 1510, NGC 1512, IC 1959, IC 1986, NGC 1448, NGC 1487, IC 1933, NGC 1311, IC 1954, IC 1914, NGC 1411, IC 1970, PGC 13818, NGC 1249, and PGC 11139.[4] And the six dropped from the 1982 list were: NGC 2082, NGC 1947, NGC 1796, NGC 1688, NGC 1672, and NGC 1559.[4] In 2007, a study of ultracompact dwarfs (UCD) identified one definite and two possible UCD members of the group.[8] The thirty-four added by Ferguson et al. 1990 included IC 2038 and IC 2039.[3]
The NGC 1566 Group of Dorado contains H I with MHI = 3.5×1010 M⊙ of which 40% alone comes from the NGC 1566 galaxy.[5] More than half of its members are outside its virial radius of 580 kpc which suggests this group is a young non-virialized group. The 2005 Kilborn et al. set of confirmed NGC 1566 Group members (within the Dorado Group) is:[5]
Name | Type[1] | R.A. (J2000)[1] | Dec. (J2000)[1] | Redshift (km/s)[1] | Apparent Magnitude[1] |
---|---|---|---|---|---|
IC 2049 | SAB(s)d? | 04h 12m 04.3s | −58° 33′ 25″ | 1469 ± 7 | 14.5 |
NGC 1536 | SB(s)c pec | 04h 10m 59.8s | −56° 28′ 50″ | 1217 ± 13 | 13.2 |
NGC 1543 | (R)SB(l)00 | 04h 12m 43.2s | −57° 44′ 17″ | 1176 ± 7 | 11.5 |
LSBG F157-081 | Irregular | 04h 27m 13.7s | −57° 25′ 42″ | 1215 ± 7 | 16.7 |
NGC 1533 | (L)SB(rs)00 | 04h 09m 51.8s | −56° 07′ 06″ | 790 ± 5 | 11.7 |
IC 2038 | Sd pec | 04h 08m 53.7s | −55° 59′ 22″ | 712 ± 52 | 15.5 |
APMBGC 157+016+068 | Irregular | 04h 22m 51.7s | −56° 13′ 39″ | 1350 ± 4 | 16.3 |
NGC 1546 | SA0+? | 04h 14m 36.5s | −56° 03′ 39″ | 1284 ± 14 | 11.8 |
IC 2058 | Sc | 04h 17m 54.3s | −55° 55′ 58″ | 1379 ± 1 | 13.9 |
IC 2032 | IAB(s)m pec | 04h 07m 03.0s | −55° 19′ 26″ | 1068 ± 7 | 14.7 |
NGC 1566 | (R'_1)SAB(rs)bcSy1 | 04h 20m 00.4s | −54° 56′ 16″ | 1504 ± 2 | 10.3 |
NGC 1596 | SA0: sp | 04h 27m 38.1s | −55° 01′ 40″ | 1510 ± 8 | 12.1 |
NGC 1602 | IB(s)m pec | 04h 27m 55.0s | −55° 03′ 28″ | 1568 ± 8 | 13.3 |
NGC 1515 | SAB(s)bc | 04h 04m 02.7s | −54° 06′ 00″ | 1175 ± 7 | 12.1 |
NGC 1522 | (R')S00: pec | 04h 06m 07.9s | −52° 40′ 06″ | 898 ± 7 | 13.9 |
ESO 118-019 | S00 pec | 04h 18m 59.5s | −58° 15′ 27″ | 1239 | 14.9 |
ESO 157-030 | E4 | 04h 27m 32.6s | −54° 11′ 48″ | 1471 ± 28 | 14.7 |
ESO 157-047 | S0/a? pec sp | 04h 39m 19.1s | −54° 12′ 41″ | 1655 ± 10 | 15.5 |
ESO 157-049 | S? | 04h 39m 36.9s | −53° 00′ 46″ | 1678 ± 5 | 14.3 |
IC 2085 | S00 pec sp | 04h 31m 24.2s | −54° 25′ 01″ | 982 ± 10 | 13.9 |
NGC 1549 | E0−1 | 04h 15m 45.1s | −55° 35′ 32″ | 1220 ± 15 | 10.7 |
NGC 1553 | SA(rl)00 | 04h 16m 10.5s | −55° 46′ 49″ | 1080 ± 11 | 10.3 |
NGC 1574 | SA0− | 04h 21m 58.8s | −56° 58′ 29″ | 1050 ± 25 | 11.4 |
NGC 1581 | S0− | 04h 24m 44.9s | −54° 56′ 31″ | 1600 ± 27 | 13.6 |
NGC 1617 | (R')SAB(rs)a | 04h 31m 39.5s | −54° 36′ 08″ | 1063 ± 21 | 11.4 |
Abell 3202 | Irregular | 04h 01m 15.2s | −53° 29′ 23″ | 1135 ± 40 | 16.9 |
External links
- The Dorado Group on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
References
- ^ a b c d e f g h i j k l "NASA/IPAC Extragalactic Database", Results for Dorado Group and various galaxies, retrieved 2008-06-26
- ^ a b c d e f g h i j Carrasco, Eleazar R.; Mendes de Oliveira, Cláudia; Infante, Leopoldo; Bolte, Michael (January 2001), "The Dwarf Galaxy Population of the Dorado Group Down to MV~−11", The Astronomical Journal, 121 (1): 148–168, arXiv:astro-ph/0010076, Bibcode:2001AJ....121..148C, doi:10.1086/318035, S2CID 1348985
- ^ a b c d e Ferguson, Henry C.; Sandage, Allan (July 1990), "Population studies in groups and clusters of galaxies. III – A catalog of galaxies in five nearby groups", Astronomical Journal, 100: 1–31, Bibcode:1990AJ....100....1F, doi:10.1086/115486, ISSN 0004-6256
- ^ a b c Maia, M. A. G.; da Costa, L. N.; Latham, David W. (April 1989), "A catalog of southern groups of galaxies", Astrophysical Journal Supplement Series, 69: 809–829, Bibcode:1989ApJS...69..809M, doi:10.1086/191328, ISSN 0067-0049
- ^ a b c d e f Virginia A. Kilborn; Bärbel S. Koribalski; Duncan A. Forbes; David G. Barnes; Ruth C. Musgrave (January 2005), "A Wide-Field Hi Study of the NGC 1566 Group", Monthly Notices of the Royal Astronomical Society, 356 (1): 77–88, arXiv:astro-ph/0409743, Bibcode:2005MNRAS.356...77K, doi:10.1111/j.1365-2966.2004.08450.x
{{citation}}
: CS1 maint: unflagged free DOI (link) - ^ a b c d e f g h Firth, P.; Evstigneeva, E. A.; Jones, J. B.; Drinkwater, M. J.; Phillipps, S.; Gregg, M. D. (November 2006), "Kinematics, substructure and luminosity-weighted dynamics of six nearby galaxy groups", Monthly Notices of the Royal Astronomical Society, 372 (4): 1856–1868, arXiv:astro-ph/0608584, Bibcode:2006MNRAS.372.1856F, doi:10.1111/j.1365-2966.2006.10993.x, S2CID 18646500
{{citation}}
: CS1 maint: unflagged free DOI (link) - ^ Laurikainen, Eija; Salo, Heikki; Buta, Ronald; Knapen, Johan; Speltincx, Tom; Block, David (December 2006), "The Near-infrared S0 Survey III: Morphology of 15 Southern Early-Type Disk Galaxies", The Astronomical Journal, 132 (6): 2634–2652, arXiv:astro-ph/0609343, Bibcode:2006AJ....132.2634L, doi:10.1086/508810, S2CID 16856632
- ^ a b Evstigneeva, E. A.; Drinkwater, M. J.; Jurek, R.; Firth, P.; Jones, J. B.; Gregg, M. D.; Phillipps, S. (July 2007), "Searches for ultracompact dwarf galaxies in galaxy groups", Monthly Notices of the Royal Astronomical Society, 378 (3): 1036–1042, arXiv:0704.1750, Bibcode:2007MNRAS.378.1036E, doi:10.1111/j.1365-2966.2007.11856.x, S2CID 15880069
{{citation}}
: CS1 maint: unflagged free DOI (link) - ^ J. L. Tonry; A. Dressler; J. P. Blakeslee; E. A. Ajhar; A. B. Fletcher; G. A. Luppino; M. R. Metzger; C. B. Moore (2001), "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances", Astrophysical Journal, 546 (2): 681–693, arXiv:astro-ph/0011223, Bibcode:2001ApJ...546..681T, doi:10.1086/318301, S2CID 17628238
- ^ a b c d DeGraaff, Regina Barber; Blakeslee, John P.; Meurer, Gerhardt R.; Putman, Mary E. (December 2007), "A Galaxy in Transition: Structure, Globular Clusters, and Distance of the Star-Forming S0 Galaxy NGC 1533 in Dorado", The Astrophysical Journal, 671 (2): 1624–1639, arXiv:0710.0893, Bibcode:2007ApJ...671.1624D, doi:10.1086/523640, S2CID 14312626
- ^ Bridges, Terry J.; Hanes, David A. (April 1990), "Globular clusters in the interacting galaxies NGC 1549 and NGC 1553", Astronomical Journal, 99: 1100–1107, 1340, 1341, Bibcode:1990AJ.....99.1100B, doi:10.1086/115399, ISSN 0004-6256
- ^ Huchra, John Peter; Geller, Margaret J. (June 15, 1982), "Groups of galaxies. I – Nearby groups", Astrophysical Journal, 257 (Part 1): 423–437, Bibcode:1982ApJ...257..423H, doi:10.1086/160000
- ^ "One from many". Retrieved 1 February 2016.