Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups
Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our projec...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Amram, P. [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2002 |
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| Schlagwörter: |
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| Anmerkung: |
© Kluwer Academic Publishers 2002 |
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| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Kluwer Academic Publishers, 1968, 281(2002), 1-2 vom: Juli, Seite 389-392 |
|---|---|
| Übergeordnetes Werk: |
volume:281 ; year:2002 ; number:1-2 ; month:07 ; pages:389-392 |
| Links: |
|---|
| DOI / URN: |
10.1023/A:1019585617481 |
|---|
| Katalog-ID: |
OLC2066232718 |
|---|
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| 520 | |a Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. | ||
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| 700 | 1 | |a Boulesteix, J. |4 aut | |
| 700 | 1 | |a Carignan, C. |4 aut | |
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10.1023/A:1019585617481 doi (DE-627)OLC2066232718 (DE-He213)A:1019585617481-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Amram, P. verfasserin aut Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups 2002 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2002 Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. Compact Group Rotation Curve Spiral Galaxy Dwarf Galaxy Dark Halo Mendes de Oliveira, C. aut Plana, H. aut Balkowski, C. aut Boulesteix, J. aut Carignan, C. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 281(2002), 1-2 vom: Juli, Seite 389-392 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:281 year:2002 number:1-2 month:07 pages:389-392 https://doi.org/10.1023/A:1019585617481 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 281 2002 1-2 07 389-392 |
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10.1023/A:1019585617481 doi (DE-627)OLC2066232718 (DE-He213)A:1019585617481-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Amram, P. verfasserin aut Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups 2002 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2002 Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. Compact Group Rotation Curve Spiral Galaxy Dwarf Galaxy Dark Halo Mendes de Oliveira, C. aut Plana, H. aut Balkowski, C. aut Boulesteix, J. aut Carignan, C. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 281(2002), 1-2 vom: Juli, Seite 389-392 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:281 year:2002 number:1-2 month:07 pages:389-392 https://doi.org/10.1023/A:1019585617481 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 281 2002 1-2 07 389-392 |
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10.1023/A:1019585617481 doi (DE-627)OLC2066232718 (DE-He213)A:1019585617481-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Amram, P. verfasserin aut Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups 2002 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2002 Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. Compact Group Rotation Curve Spiral Galaxy Dwarf Galaxy Dark Halo Mendes de Oliveira, C. aut Plana, H. aut Balkowski, C. aut Boulesteix, J. aut Carignan, C. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 281(2002), 1-2 vom: Juli, Seite 389-392 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:281 year:2002 number:1-2 month:07 pages:389-392 https://doi.org/10.1023/A:1019585617481 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 281 2002 1-2 07 389-392 |
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10.1023/A:1019585617481 doi (DE-627)OLC2066232718 (DE-He213)A:1019585617481-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Amram, P. verfasserin aut Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups 2002 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2002 Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. Compact Group Rotation Curve Spiral Galaxy Dwarf Galaxy Dark Halo Mendes de Oliveira, C. aut Plana, H. aut Balkowski, C. aut Boulesteix, J. aut Carignan, C. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 281(2002), 1-2 vom: Juli, Seite 389-392 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:281 year:2002 number:1-2 month:07 pages:389-392 https://doi.org/10.1023/A:1019585617481 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 281 2002 1-2 07 389-392 |
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10.1023/A:1019585617481 doi (DE-627)OLC2066232718 (DE-He213)A:1019585617481-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Amram, P. verfasserin aut Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups 2002 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2002 Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. Compact Group Rotation Curve Spiral Galaxy Dwarf Galaxy Dark Halo Mendes de Oliveira, C. aut Plana, H. aut Balkowski, C. aut Boulesteix, J. aut Carignan, C. aut Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 281(2002), 1-2 vom: Juli, Seite 389-392 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:281 year:2002 number:1-2 month:07 pages:389-392 https://doi.org/10.1023/A:1019585617481 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 281 2002 1-2 07 389-392 |
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520 530 620 VZ 16,12 ssgn Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups Compact Group Rotation Curve Spiral Galaxy Dwarf Galaxy Dark Halo |
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Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups |
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Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups |
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Amram, P. |
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Astrophysics and space science |
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Amram, P. Mendes de Oliveira, C. Plana, H. Balkowski, C. Boulesteix, J. Carignan, C. |
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kinematics and dynamics of galaxies in compact groups for a sample of 31 groups |
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Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups |
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Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. © Kluwer Academic Publishers 2002 |
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Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. © Kluwer Academic Publishers 2002 |
| abstract_unstemmed |
Abstract A long-term program based on Fabry-Perot Hα velocity field data of compact groups has been undertaken in order to analyse the kinematics of the compact group galaxies and the extent of their dark halos. The data are taken at the ESO and the CFH 3.6 m telescopes. The main goals of our project are: • To determine the evolutionary stages of the studied groups, • To search for tidal dwarf galaxy candidates in heavily interacting systems and • in combination with photometry available in the literature, to determine the Tully-Fisher relation for the group galaxies. The sample contains examples of groups at a variety of dynamical stages: from a false group that is in fact one single irregular galaxy with several star-forming blobs (e.g. H18) to a group whose members are strongly interacting and possibly forming tidal dwarf galaxies (e.g. H92) to a group in the final process of merging. We have so far identified five HCG classes: 1. merging groups2. strongly interacting, 3. weakly interacting, 4. non-groups, 5. single irregular galaxies. The ones which can be used in the TF studies are those in classes (2) and (3), for which comprehensive rotation curves can be derived. © Kluwer Academic Publishers 2002 |
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Kinematics and Dynamics of Galaxies in Compact Groups for a sample of 31 groups |
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