The AMIGA sample of isolated galaxies. XIV. Disc breaks and interactions through ultra-deep optical imaging Article Swipe
P. M. Sánchez-Alarcón
,
Javier Román
,
J. H. Knapen
,
L. Verdes‐Montenegro
,
S. Comerón
,
R. M. Rich
,
J. E. Beckman
,
M. Argudo–Fernández
,
P. Ramírez-Moreta
,
Javier Abad Blasco
,
E. Unda-Sanzana
,
Julián Garrido
,
S. Sánchez–Expósito
·
YOU?
·
· 2023
· Open Access
·
· DOI: https://doi.org/10.48550/arxiv.2307.02527
YOU?
·
· 2023
· Open Access
·
· DOI: https://doi.org/10.48550/arxiv.2307.02527
In the standard cosmological model of galaxy evolution, mergers and interactions play a fundamental role in shaping galaxies. Galaxies that are currently isolated are thus interesting, allowing us to distinguish between internal and external processes affecting the galactic structure. However, current observational limits may obscure crucial information in the low-mass or low-brightness regime. We use optical imaging of a subsample of the AMIGA catalogue of isolated galaxies to explore the impact of different factors on the structure of these galaxies. We study the type of disc break as a function of the degree of isolation and the presence of interaction indicators like tidal streams or plumes only detectable in the low surface brightness regime. We present deep optical imaging of a sample of 25 isolated galaxies. Through careful data processing and analysis techniques, the surface brightness limits achieved are comparable to those to be obtained on the 10-year LSST coadds. The extreme depth of our imaging allows us to study the interaction signatures of 20 galaxies, given that the presence of Galactic cirrus is a strong limiting factor in the characterisation of interactions for the remaining 5 of them. We detect previously unreported interaction features in 8 (40%) galaxies in our sample. We identify 9 galaxies (36%) showing an exponential disc (Type I), 14 galaxies (56%) with down-bending (Type II) profile and only 2 galaxies (8%) with up-bending (Type III) profiles. Isolated galaxies have considerably more purely exponential discs and fewer up-bending surface brightness profiles than field or cluster galaxies. We suggest that major mergers produce up-bending profiles while a threshold in star formation probably forms down-bending profiles. Unperturbed galaxies, evolving slowly with a low star formation rate could cause the high rate of Type I discs in isolated galaxies observed.
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Metadata
- Type
- preprint
- Language
- en
- Landing Page
- http://arxiv.org/abs/2307.02527
- https://arxiv.org/pdf/2307.02527
- OA Status
- green
- Related Works
- 10
- OpenAlex ID
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All OpenAlex metadata
Raw OpenAlex JSON
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https://openalex.org/W4383604301Canonical identifier for this work in OpenAlex
- DOI
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https://doi.org/10.48550/arxiv.2307.02527Digital Object Identifier
- Title
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The AMIGA sample of isolated galaxies. XIV. Disc breaks and interactions through ultra-deep optical imagingWork title
- Type
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preprintOpenAlex work type
- Language
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enPrimary language
- Publication year
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2023Year of publication
- Publication date
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2023-07-05Full publication date if available
- Authors
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P. M. Sánchez-Alarcón, Javier Román, J. H. Knapen, L. Verdes‐Montenegro, S. Comerón, R. M. Rich, J. E. Beckman, M. Argudo–Fernández, P. Ramírez-Moreta, Javier Abad Blasco, E. Unda-Sanzana, Julián Garrido, S. Sánchez–ExpósitoList of authors in order
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https://arxiv.org/abs/2307.02527Publisher landing page
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https://arxiv.org/pdf/2307.02527Direct link to full text PDF
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YesWhether a free full text is available
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greenOpen access status per OpenAlex
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Physics, Astrophysics, Surface brightness, Galaxy, Astronomy, Disc, Elliptical galaxyTop concepts (fields/topics) attached by OpenAlex
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0Total citation count in OpenAlex
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10Other works algorithmically related by OpenAlex
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| abstract_inverted_index.purely | 236 |
| abstract_inverted_index.sample | 121 |
| abstract_inverted_index.slowly | 271 |
| abstract_inverted_index.strong | 175 |
| abstract_inverted_index.10-year | 147 |
| abstract_inverted_index.Through | 126 |
| abstract_inverted_index.between | 30 |
| abstract_inverted_index.careful | 127 |
| abstract_inverted_index.cluster | 248 |
| abstract_inverted_index.coadds. | 149 |
| abstract_inverted_index.crucial | 45 |
| abstract_inverted_index.current | 40 |
| abstract_inverted_index.explore | 68 |
| abstract_inverted_index.extreme | 151 |
| abstract_inverted_index.factors | 73 |
| abstract_inverted_index.imaging | 56, 118, 155 |
| abstract_inverted_index.mergers | 8, 254 |
| abstract_inverted_index.obscure | 44 |
| abstract_inverted_index.optical | 55, 117 |
| abstract_inverted_index.present | 115 |
| abstract_inverted_index.produce | 255 |
| abstract_inverted_index.profile | 220 |
| abstract_inverted_index.regime. | 52, 113 |
| abstract_inverted_index.sample. | 201 |
| abstract_inverted_index.shaping | 16 |
| abstract_inverted_index.showing | 207 |
| abstract_inverted_index.streams | 103 |
| abstract_inverted_index.suggest | 251 |
| abstract_inverted_index.surface | 111, 134, 242 |
| abstract_inverted_index.Galactic | 171 |
| abstract_inverted_index.Galaxies | 18 |
| abstract_inverted_index.However, | 39 |
| abstract_inverted_index.Isolated | 231 |
| abstract_inverted_index.achieved | 137 |
| abstract_inverted_index.allowing | 26 |
| abstract_inverted_index.analysis | 131 |
| abstract_inverted_index.evolving | 270 |
| abstract_inverted_index.external | 33 |
| abstract_inverted_index.features | 194 |
| abstract_inverted_index.function | 89 |
| abstract_inverted_index.galactic | 37 |
| abstract_inverted_index.galaxies | 66, 198, 205, 214, 224, 232, 289 |
| abstract_inverted_index.identify | 203 |
| abstract_inverted_index.internal | 31 |
| abstract_inverted_index.isolated | 22, 65, 124, 288 |
| abstract_inverted_index.limiting | 176 |
| abstract_inverted_index.low-mass | 49 |
| abstract_inverted_index.obtained | 144 |
| abstract_inverted_index.presence | 97, 169 |
| abstract_inverted_index.probably | 264 |
| abstract_inverted_index.profiles | 244, 257 |
| abstract_inverted_index.standard | 2 |
| abstract_inverted_index.affecting | 35 |
| abstract_inverted_index.catalogue | 63 |
| abstract_inverted_index.currently | 21 |
| abstract_inverted_index.different | 72 |
| abstract_inverted_index.formation | 263, 276 |
| abstract_inverted_index.galaxies, | 165, 269 |
| abstract_inverted_index.galaxies. | 17, 79, 125, 249 |
| abstract_inverted_index.isolation | 94 |
| abstract_inverted_index.observed. | 290 |
| abstract_inverted_index.processes | 34 |
| abstract_inverted_index.profiles. | 230, 267 |
| abstract_inverted_index.remaining | 185 |
| abstract_inverted_index.structure | 76 |
| abstract_inverted_index.subsample | 59 |
| abstract_inverted_index.threshold | 260 |
| abstract_inverted_index.brightness | 112, 135, 243 |
| abstract_inverted_index.comparable | 139 |
| abstract_inverted_index.detectable | 107 |
| abstract_inverted_index.evolution, | 7 |
| abstract_inverted_index.indicators | 100 |
| abstract_inverted_index.previously | 191 |
| abstract_inverted_index.processing | 129 |
| abstract_inverted_index.signatures | 162 |
| abstract_inverted_index.structure. | 38 |
| abstract_inverted_index.unreported | 192 |
| abstract_inverted_index.up-bending | 227, 241, 256 |
| abstract_inverted_index.Unperturbed | 268 |
| abstract_inverted_index.distinguish | 29 |
| abstract_inverted_index.exponential | 209, 237 |
| abstract_inverted_index.fundamental | 13 |
| abstract_inverted_index.information | 46 |
| abstract_inverted_index.interaction | 99, 161, 193 |
| abstract_inverted_index.techniques, | 132 |
| abstract_inverted_index.considerably | 234 |
| abstract_inverted_index.cosmological | 3 |
| abstract_inverted_index.down-bending | 217, 266 |
| abstract_inverted_index.interactions | 10, 182 |
| abstract_inverted_index.interesting, | 25 |
| abstract_inverted_index.observational | 41 |
| abstract_inverted_index.low-brightness | 51 |
| abstract_inverted_index.characterisation | 180 |
| cited_by_percentile_year | |
| countries_distinct_count | 0 |
| institutions_distinct_count | 13 |
| citation_normalized_percentile.value | 0.11972262 |
| citation_normalized_percentile.is_in_top_1_percent | False |
| citation_normalized_percentile.is_in_top_10_percent | False |