{"id":{"repo_id":"ull","oai_identifier":"oai:riull.ull.es:915/25756"},"canonical_url":"https://search.dev.ndltd.org/etd/ull/oai:riull.ull.es:915/25756","repository":{"repo_id":"ull","name":"Universidad de la Laguna","base_url":"https://riull.ull.es/oai/request"},"display":{"title":"Morphology and metallicities of OTELO galaxies.","abstract":"In this thesis we explore the OTELO (OSIRIS Tunable Filter Emission Line Object) survey. OTELO is a very deep, pencil beam survey for the search of emission line sources by means of the tunable filters of the OSIRIS instrument, installed at the Gran Telescopio Canarias. A tomography scan method results in 2D, low-resolution pseudo-spectra for all the sources in the observed field. The reached line flux of 4:6 10^19 erg s^-1 cm^2 makes it the deepest survey in terms of the line flux. In particular, we present the morphological catalogue of the OTELO sources detected in high-resolution images from the ACS instrument of the Hubble Space Telescope. We have employed a parametric method to fit 2D model composed of single-Sérsic profile using a multi-wavelength version of GALFIT software. This software fits simultaneously selected model to all given images using Chebyshev polynomial functions. We show that this multi-wavelength method provides better results in the low signal-to-noise, recovering a substantial fraction of sources in this regime, as compared to a standard version of the same software. We also provide a preliminary visual morphology of the selected sample (up to magnitude I=24.5 mag). The results of this analysis are consistent with the obtained from the parametric method. We have tested various methods for separation of early-type galaxies from late-type galaxies, as well as the mass-size relation. We also found a median stellar mass evolution up to z = 2 finding good agreement with previous works. From the morphological catalogue we selected a population of early-type emission line galaxies (ET-ELG). Even if under investigation for many decades, there is lack of the clear consensus on the nature and origin of the emission lines found in the ET-ELG. We study a sample of 14 such objects at intermediate redshift. Due to the limited spectral information available, we compared the number densities of our sample with a carefully selected sample of local counterparts from SDSS. We found that OTELO detects a considerably higher ET-ELG density than it would be expected from the local SDSS sample. This result holds even considering a cosmic variance – the most important source of uncertainties for a pencil beam survey ( 56 arcmin^2) as OTELO. Finally, we studied a stellar-mass–metallicity relation (MZR) of selected Ha emission line sources at z~0.4. Particularly, and taking advantage of the depth reached by the OTELO survey, we focus on the very low-mass end of this relation, with the low-mass limit (10^7Msun ). Most of the galaxies in the Ha sample are morphologically classified as disk-like sources with low Sérsic index, as expected for the star-forming galaxies. We have found no evidence for the evolution of the MZR since z = 0.4.","abstract_html":"In this thesis we explore the OTELO (OSIRIS Tunable Filter Emission Line Object) survey. OTELO is a very deep, pencil beam survey for the search of emission line sources by means of the tunable filters of the OSIRIS instrument, installed at the Gran Telescopio Canarias. A tomography scan method results in 2D, low-resolution pseudo-spectra for all the sources in the observed field. The reached line flux of 4:6 10^19 erg s^-1 cm^2 makes it the deepest survey in terms of the line flux. In particular, we present the morphological catalogue of the OTELO sources detected in high-resolution images from the ACS instrument of the Hubble Space Telescope. We have employed a parametric method to fit 2D model composed of single-Sérsic profile using a multi-wavelength version of GALFIT software. This software fits simultaneously selected model to all given images using Chebyshev polynomial functions. We show that this multi-wavelength method provides better results in the low signal-to-noise, recovering a substantial fraction of sources in this regime, as compared to a standard version of the same software. We also provide a preliminary visual morphology of the selected sample (up to magnitude I=24.5 mag). The results of this analysis are consistent with the obtained from the parametric method. We have tested various methods for separation of early-type galaxies from late-type galaxies, as well as the mass-size relation. We also found a median stellar mass evolution up to z = 2 finding good agreement with previous works. From the morphological catalogue we selected a population of early-type emission line galaxies (ET-ELG). Even if under investigation for many decades, there is lack of the clear consensus on the nature and origin of the emission lines found in the ET-ELG. We study a sample of 14 such objects at intermediate redshift. Due to the limited spectral information available, we compared the number densities of our sample with a carefully selected sample of local counterparts from SDSS. We found that OTELO detects a considerably higher ET-ELG density than it would be expected from the local SDSS sample. This result holds even considering a cosmic variance – the most important source of uncertainties for a pencil beam survey ( 56 arcmin^2) as OTELO. Finally, we studied a stellar-mass–metallicity relation (MZR) of selected Ha emission line sources at z~0.4. Particularly, and taking advantage of the depth reached by the OTELO survey, we focus on the very low-mass end of this relation, with the low-mass limit (10^7Msun ). Most of the galaxies in the Ha sample are morphologically classified as disk-like sources with low Sérsic index, as expected for the star-forming galaxies. We have found no evidence for the evolution of the MZR since z = 0.4.","abstract_has_math":false,"creators":["Nadolny, Jakub"],"institution":null,"degree_name":null,"degree_level":null,"degree_discipline":null,"degree_department":null,"school":null,"contributors":[],"advisors":["Cepa Nogue, Jorge","Cerviño Saavedra, Miguel Antonio","Bongiovanni Pérez, Ángel Manuel"],"committee_chairs":[],"committee_members":[],"year":2021,"date_issued":"2021","date_published":"2021","updated_at":"2026-08-21T16:49:21Z","subjects":[],"languages":["en"],"rights":["Attribution-NonCommercial-NoDerivatives 4.0 Internacional"],"rights_urls":["http://creativecommons.org/licenses/by-nc-nd/4.0/"],"identifier_entries":[{"key":"dc:identifier","label":"Identifier","values":["hdl:915/25756"],"render_values":[{"text":"hdl:915/25756","href":null,"code":true}]}]},"links":{"outbound_url":"http://riull.ull.es/xmlui/handle/915/25756","outbound_label":"Repository record","outbound_source":"dc:identifier.uri"},"source_record":{"url":"https://riull.ull.es/oai/request?verb=GetRecord&metadataPrefix=dim&identifier=oai%3Ariull.ull.es%3A915%2F25756","prefix":"dim"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor.advisor","label":"Advisor","values":["Cepa Nogue, Jorge","Cerviño Saavedra, Miguel Antonio","Bongiovanni Pérez, Ángel Manuel"]},{"key":"dc:contributor.other","label":"Dc Contributor Other","values":["Programa de Doctorado en Astrofísica"]},{"key":"dc:creator","label":"Author","values":["Nadolny, Jakub"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date.accessioned","label":"Dc Date Accessioned","values":["2021-10-26T07:49:47Z"]},{"key":"dc:date.available","label":"Dc Date Available","values":["2021-10-26T07:49:47Z"]},{"key":"dc:date.issued","label":"Date","values":["2021"]},{"key":"dc:type","label":"Dc Type","values":["info:eu-repo/semantics/doctoralThesis"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language.iso","label":"Language (ISO)","values":["en"]},{"key":"dc:rights","label":"Dc Rights","values":["Attribution-NonCommercial-NoDerivatives 4.0 Internacional"]},{"key":"dc:rights.uri","label":"Rights URI","values":["http://creativecommons.org/licenses/by-nc-nd/4.0/"]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier","label":"Identifier","values":["hdl:915/25756"]},{"key":"dc:identifier.uri","label":"Identifier URI","values":["http://riull.ull.es/xmlui/handle/915/25756"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description.abstract","label":"Abstract","values":["In this thesis we explore the OTELO (OSIRIS Tunable Filter Emission Line Object) survey. OTELO is a very deep, pencil beam survey for the search of emission line sources by means of the tunable filters of the OSIRIS instrument, installed at the Gran Telescopio Canarias. A tomography scan method results in 2D, low-resolution pseudo-spectra for all the sources in the observed field. The reached line flux of 4:6 10^19 erg s^-1 cm^2 makes it the deepest survey in terms of the line flux. In particular, we present the morphological catalogue of the OTELO sources detected in high-resolution images from the ACS instrument of the Hubble Space Telescope. We have employed a parametric method to fit 2D model composed of single-Sérsic profile using a multi-wavelength version of GALFIT software. This software fits simultaneously selected model to all given images using Chebyshev polynomial functions. We show that this multi-wavelength method provides better results in the low signal-to-noise, recovering a substantial fraction of sources in this regime, as compared to a standard version of the same software. We also provide a preliminary visual morphology of the selected sample (up to magnitude I=24.5 mag). The results of this analysis are consistent with the obtained from the parametric method. We have tested various methods for separation of early-type galaxies from late-type galaxies, as well as the mass-size relation. We also found a median stellar mass evolution up to z = 2 finding good agreement with previous works. From the morphological catalogue we selected a population of early-type emission line galaxies (ET-ELG). Even if under investigation for many decades, there is lack of the clear consensus on the nature and origin of the emission lines found in the ET-ELG. We study a sample of 14 such objects at intermediate redshift. Due to the limited spectral information available, we compared the number densities of our sample with a carefully selected sample of local counterparts from SDSS. We found that OTELO detects a considerably higher ET-ELG density than it would be expected from the local SDSS sample. This result holds even considering a cosmic variance – the most important source of uncertainties for a pencil beam survey ( 56 arcmin^2) as OTELO. Finally, we studied a stellar-mass–metallicity relation (MZR) of selected Ha emission line sources at z~0.4. Particularly, and taking advantage of the depth reached by the OTELO survey, we focus on the very low-mass end of this relation, with the low-mass limit (10^7Msun ). Most of the galaxies in the Ha sample are morphologically classified as disk-like sources with low Sérsic index, as expected for the star-forming galaxies. We have found no evidence for the evolution of the MZR since z = 0.4."]},{"key":"dc:description.other","label":"Dc Description Other","values":["In this thesis we explore the OTELO (OSIRIS Tunable Filter Emission Line Object) survey. OTELO is a very deep, pencil beam survey for the search of emission line sources by means of the tunable filters of the OSIRIS instrument, installed at the Gran Telescopio Canarias. A tomography scan method results in 2D, low-resolution pseudo-spectra for all the sources in the observed field. The reached line flux of 4:6 10^19 erg s^-1 cm^2 makes it the deepest survey in terms of the line flux. In particular, we present the morphological catalogue of the OTELO sources detected in high-resolution images from the ACS instrument of the Hubble Space Telescope. We have employed a parametric method to fit 2D model composed of single-Sérsic profile using a multi-wavelength version of GALFIT software. This software fits simultaneously selected model to all given images using Chebyshev polynomial functions. We show that this multi-wavelength method provides better results in the low signal-to-noise, recovering a substantial fraction of sources in this regime, as compared to a standard version of the same software. We also provide a preliminary visual morphology of the selected sample (up to magnitude I=24.5 mag). The results of this analysis are consistent with the obtained from the parametric method. We have tested various methods for separation of early-type galaxies from late-type galaxies, as well as the mass-size relation. We also found a median stellar mass evolution up to z = 2 finding good agreement with previous works. From the morphological catalogue we selected a population of early-type emission line galaxies (ET-ELG). Even if under investigation for many decades, there is lack of the clear consensus on the nature and origin of the emission lines found in the ET-ELG. We study a sample of 14 such objects at intermediate redshift. Due to the limited spectral information available, we compared the number densities of our sample with a carefully selected sample of local counterparts from SDSS. We found that OTELO detects a considerably higher ET-ELG density than it would be expected from the local SDSS sample. This result holds even considering a cosmic variance – the most important source of uncertainties for a pencil beam survey ( 56 arcmin^2) as OTELO. Finally, we studied a stellar-mass–metallicity relation (MZR) of selected Ha emission line sources at z~0.4. Particularly, and taking advantage of the depth reached by the OTELO survey, we focus on the very low-mass end of this relation, with the low-mass limit (10^7Msun ). Most of the galaxies in the Ha sample are morphologically classified as disk-like sources with low Sérsic index, as expected for the star-forming galaxies. We have found no evidence for the evolution of the MZR since z = 0.4."]},{"key":"dc:format.mimetype","label":"Dc Format Mimetype","values":["application/pdf"]},{"key":"dc:title","label":"Title","values":["Morphology and metallicities of OTELO galaxies."]}]}],"canonical_facts":{"dc:contributor.advisor":["Cepa Nogue, Jorge","Cerviño Saavedra, Miguel Antonio","Bongiovanni Pérez, Ángel Manuel"],"dc:contributor.other":["Programa de Doctorado en Astrofísica"],"dc:creator":["Nadolny, Jakub"],"dc:date.accessioned":["2021-10-26T07:49:47Z"],"dc:date.available":["2021-10-26T07:49:47Z"],"dc:date.issued":["2021"],"dc:description.abstract":["In this thesis we explore the OTELO (OSIRIS Tunable Filter Emission Line Object) survey. OTELO is a very deep, pencil beam survey for the search of emission line sources by means of the tunable filters of the OSIRIS instrument, installed at the Gran Telescopio Canarias. A tomography scan method results in 2D, low-resolution pseudo-spectra for all the sources in the observed field. The reached line flux of 4:6 10^19 erg s^-1 cm^2 makes it the deepest survey in terms of the line flux. In particular, we present the morphological catalogue of the OTELO sources detected in high-resolution images from the ACS instrument of the Hubble Space Telescope. We have employed a parametric method to fit 2D model composed of single-Sérsic profile using a multi-wavelength version of GALFIT software. This software fits simultaneously selected model to all given images using Chebyshev polynomial functions. We show that this multi-wavelength method provides better results in the low signal-to-noise, recovering a substantial fraction of sources in this regime, as compared to a standard version of the same software. We also provide a preliminary visual morphology of the selected sample (up to magnitude I=24.5 mag). The results of this analysis are consistent with the obtained from the parametric method. We have tested various methods for separation of early-type galaxies from late-type galaxies, as well as the mass-size relation. We also found a median stellar mass evolution up to z = 2 finding good agreement with previous works. From the morphological catalogue we selected a population of early-type emission line galaxies (ET-ELG). Even if under investigation for many decades, there is lack of the clear consensus on the nature and origin of the emission lines found in the ET-ELG. We study a sample of 14 such objects at intermediate redshift. Due to the limited spectral information available, we compared the number densities of our sample with a carefully selected sample of local counterparts from SDSS. We found that OTELO detects a considerably higher ET-ELG density than it would be expected from the local SDSS sample. This result holds even considering a cosmic variance – the most important source of uncertainties for a pencil beam survey ( 56 arcmin^2) as OTELO. Finally, we studied a stellar-mass–metallicity relation (MZR) of selected Ha emission line sources at z~0.4. Particularly, and taking advantage of the depth reached by the OTELO survey, we focus on the very low-mass end of this relation, with the low-mass limit (10^7Msun ). Most of the galaxies in the Ha sample are morphologically classified as disk-like sources with low Sérsic index, as expected for the star-forming galaxies. We have found no evidence for the evolution of the MZR since z = 0.4."],"dc:description.other":["In this thesis we explore the OTELO (OSIRIS Tunable Filter Emission Line Object) survey. OTELO is a very deep, pencil beam survey for the search of emission line sources by means of the tunable filters of the OSIRIS instrument, installed at the Gran Telescopio Canarias. A tomography scan method results in 2D, low-resolution pseudo-spectra for all the sources in the observed field. The reached line flux of 4:6 10^19 erg s^-1 cm^2 makes it the deepest survey in terms of the line flux. In particular, we present the morphological catalogue of the OTELO sources detected in high-resolution images from the ACS instrument of the Hubble Space Telescope. We have employed a parametric method to fit 2D model composed of single-Sérsic profile using a multi-wavelength version of GALFIT software. This software fits simultaneously selected model to all given images using Chebyshev polynomial functions. We show that this multi-wavelength method provides better results in the low signal-to-noise, recovering a substantial fraction of sources in this regime, as compared to a standard version of the same software. We also provide a preliminary visual morphology of the selected sample (up to magnitude I=24.5 mag). The results of this analysis are consistent with the obtained from the parametric method. We have tested various methods for separation of early-type galaxies from late-type galaxies, as well as the mass-size relation. We also found a median stellar mass evolution up to z = 2 finding good agreement with previous works. From the morphological catalogue we selected a population of early-type emission line galaxies (ET-ELG). Even if under investigation for many decades, there is lack of the clear consensus on the nature and origin of the emission lines found in the ET-ELG. We study a sample of 14 such objects at intermediate redshift. Due to the limited spectral information available, we compared the number densities of our sample with a carefully selected sample of local counterparts from SDSS. We found that OTELO detects a considerably higher ET-ELG density than it would be expected from the local SDSS sample. This result holds even considering a cosmic variance – the most important source of uncertainties for a pencil beam survey ( 56 arcmin^2) as OTELO. Finally, we studied a stellar-mass–metallicity relation (MZR) of selected Ha emission line sources at z~0.4. Particularly, and taking advantage of the depth reached by the OTELO survey, we focus on the very low-mass end of this relation, with the low-mass limit (10^7Msun ). Most of the galaxies in the Ha sample are morphologically classified as disk-like sources with low Sérsic index, as expected for the star-forming galaxies. We have found no evidence for the evolution of the MZR since z = 0.4."],"dc:format.mimetype":["application/pdf"],"dc:identifier":["hdl:915/25756"],"dc:identifier.uri":["http://riull.ull.es/xmlui/handle/915/25756"],"dc:language.iso":["en"],"dc:rights":["Attribution-NonCommercial-NoDerivatives 4.0 Internacional"],"dc:rights.uri":["http://creativecommons.org/licenses/by-nc-nd/4.0/"],"dc:title":["Morphology and metallicities of OTELO galaxies."],"dc:type":["info:eu-repo/semantics/doctoralThesis"]},"updated_at":"2026-08-21T16:49:21Z"}