Cairós, Luz Marina

[["dc.bibliographiccitation.firstpage","A119"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","608"],["dc.contributor.author","Cairós, L. M."],["dc.contributor.author","González-Pérez, J. N."],["dc.date.accessioned","2020-12-10T18:11:36Z"],["dc.date.available","2020-12-10T18:11:36Z"],["dc.date.issued","2017"],["dc.identifier.doi","10.1051/0004-6361/201731293"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74079"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Probing star formation and feedback in dwarf galaxies"],["dc.title.alternative","Integral field view of the blue compact galaxy Tololo 1937-423⋆"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A95"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","634"],["dc.contributor.author","Cairós, L. M."],["dc.contributor.author","González-Pérez, J. N."],["dc.date.accessioned","2020-12-10T18:11:52Z"],["dc.date.available","2020-12-10T18:11:52Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1051/0004-6361/201936174"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74166"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Understanding star formation and feedback in small galaxies"],["dc.title.alternative","The case of the blue compact dwarf Mrk 900"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A125"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","600"],["dc.contributor.author","Cairós, L. M."],["dc.contributor.author","González-Pérez, J. N."],["dc.date.accessioned","2020-12-10T18:11:34Z"],["dc.date.available","2020-12-10T18:11:34Z"],["dc.date.issued","2017"],["dc.identifier.doi","10.1051/0004-6361/201629681"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74061"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Integral field observations of the blue compact galaxy Haro14"],["dc.title.alternative","Star formation and feedback in dwarf galaxies"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A144"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","664"],["dc.contributor.author","Cairós, L. M."],["dc.contributor.author","González-Pérez, J. N."],["dc.contributor.author","Weilbacher, P. M."],["dc.contributor.author","Manso Sainz, R."],["dc.date.accessioned","2022-10-04T10:21:05Z"],["dc.date.available","2022-10-04T10:21:05Z"],["dc.date.issued","2022"],["dc.description.abstract","We investigate the warm ionized gas in the blue compact galaxy (BCG) Haro 14 by means of integral field spectroscopic observations taken with the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope. The large field of view of MUSE and its unprecedented sensitivity enable observations of the galaxy nebular emission up to large galactocentric distances, even in the important but very faint [O \n I\n ]\n λ\n 6300 diagnostic line. This allowed us to trace the ionized gas morphology and ionization structure of Haro 14 up to kiloparsec scales and, for the first time, to accurately investigate the excitation mechanism operating in the outskirts of a typical BCG. The intensity and diagnostic maps reveal at least two highly distinct components of ionized gas: the bright central regions, mostly made of individual clumps, and a faint component which extends up to kiloparsec scales and consists of widespread diffuse emission, well-delineated filamentary structures, and faint knots. Noteworthy are the two curvilinear filaments extending up to 2 and 2.3 kpc southwest, which likely trace the edges of supergiant expanding bubbles driven by galactic outflows. We find that while the central clumps in Haro 14 are H \n II\n -region complexes, the morphology and line ratios of the whole low-surface-brightness component are not compatible with star formation photoionization. In the spatially resolved emission-line-ratio diagnostic diagrams, spaxels above the maximum starburst line form the majority (∼75% and ∼50% in the diagnostic diagrams involving [O \n I\n ] and [S \n II\n ] respectively). Moreover, our findings suggest that more than one alternative mechanism is ionizing the outer galaxy regions. The properties of the diffuse component are consistent with ionization by diluted radiation and the large filaments and shells are most probably shocked areas at the edge of bubbles. The mechanism responsible for the ionization of the faint individual clumps observed in the galaxy periphery is more difficult to assess. These clumps could be the shocked debris of fragmented shells or regions where star formation is proceeding under extreme conditions."],["dc.identifier.doi","10.1051/0004-6361/202243028"],["dc.identifier.pii","aa43028-22"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/114328"],["dc.notes.intern","DOI-Import GROB-600"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","Warm ionized gas in the blue compact galaxy Haro 14 viewed by MUSE"],["dc.title.alternative","The diverse ionization mechanisms acting in low-mass starbursts"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A142"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","654"],["dc.contributor.author","Cairós, Luz Marina"],["dc.contributor.author","González-Pérez, J. N."],["dc.contributor.author","Weilbacher, P. M."],["dc.contributor.author","Manso Sainz, R."],["dc.date.accessioned","2021-12-01T09:20:57Z"],["dc.date.available","2021-12-01T09:20:57Z"],["dc.date.issued","2021"],["dc.description.abstract","Investigations of blue compact galaxies (BCGs) are essential to advancing our understanding of galaxy formation and evolution. BCGs are low-luminosity, low-metallicity, gas-rich objects that form stars at extremely high rates, meaning they are good analogs to the high-redshift star-forming galaxy population. Being low-mass starburst systems, they also constitute excellent laboratories in which to investigate the star formation process and the interplay between massive stars and their surroundings. This work presents results from integral field spectroscopic observations of the BCG Haro 14 taken with the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope in wide-field adaptive optics mode. The large MUSE field of view (1′×1′ = 3.8 × 3.8 kpc 2 at the adopted distance of 13 Mpc) enables simultaneous observations of the central starburst and the low-surface-brightness host galaxy, which is a huge improvement with respect to previous integral field spectroscopy of BCGs. From these data we built galaxy maps in continuum and in the brightest emission lines. We also generated synthetic broad-band images in the VRI bands, from which we produced color index maps and surface brightness profiles. We detected numerous clumps spread throughout the galaxy, both in continuum and in emission lines, and produced a catalog with their position, size, and photometry. This analysis allowed us to study the morphology and stellar populations of Haro 14 in detail. The stellar distribution shows a pronounced asymmetry; the intensity peak in continuum is not centered with respect to the underlying stellar host but is displaced by about 500 pc southwest. At the position of the continuum peak we find a bright stellar cluster that with M v  = −12.18 appears as a strong super stellar cluster candidate. We also find a highly asymmetric, blue, but nonionizing stellar component that occupies almost the whole eastern part of the galaxy. We conclude that there are at least three different stellar populations in Haro 14: the current starburst of about 6 Myr; an intermediate-age component of between ten and several hundred million years; and a red and regular host of several gigayears. The pronounced lopsidedness in the continuum and also in the color maps, and the presence of numerous stellar clusters, are consistent with a scenario of mergers or interactions acting in Haro 14."],["dc.description.abstract","Investigations of blue compact galaxies (BCGs) are essential to advancing our understanding of galaxy formation and evolution. BCGs are low-luminosity, low-metallicity, gas-rich objects that form stars at extremely high rates, meaning they are good analogs to the high-redshift star-forming galaxy population. Being low-mass starburst systems, they also constitute excellent laboratories in which to investigate the star formation process and the interplay between massive stars and their surroundings. This work presents results from integral field spectroscopic observations of the BCG Haro 14 taken with the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope in wide-field adaptive optics mode. The large MUSE field of view (1′×1′ = 3.8 × 3.8 kpc 2 at the adopted distance of 13 Mpc) enables simultaneous observations of the central starburst and the low-surface-brightness host galaxy, which is a huge improvement with respect to previous integral field spectroscopy of BCGs. From these data we built galaxy maps in continuum and in the brightest emission lines. We also generated synthetic broad-band images in the VRI bands, from which we produced color index maps and surface brightness profiles. We detected numerous clumps spread throughout the galaxy, both in continuum and in emission lines, and produced a catalog with their position, size, and photometry. This analysis allowed us to study the morphology and stellar populations of Haro 14 in detail. The stellar distribution shows a pronounced asymmetry; the intensity peak in continuum is not centered with respect to the underlying stellar host but is displaced by about 500 pc southwest. At the position of the continuum peak we find a bright stellar cluster that with M v  = −12.18 appears as a strong super stellar cluster candidate. We also find a highly asymmetric, blue, but nonionizing stellar component that occupies almost the whole eastern part of the galaxy. We conclude that there are at least three different stellar populations in Haro 14: the current starburst of about 6 Myr; an intermediate-age component of between ten and several hundred million years; and a red and regular host of several gigayears. The pronounced lopsidedness in the continuum and also in the color maps, and the presence of numerous stellar clusters, are consistent with a scenario of mergers or interactions acting in Haro 14."],["dc.identifier.doi","10.1051/0004-6361/202140396"],["dc.identifier.pii","aa40396-21"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/94310"],["dc.notes.intern","DOI-Import GROB-478"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.rights.uri","https://www.edpsciences.org/en/authors/copyright-and-licensing"],["dc.title","MUSE observations of the blue compact dwarf galaxy Haro 14"],["dc.title.alternative","Data analysis and first results on morphology and stellar populations"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]