Browsing by Author "Aquino-Ortiz, E."

Now showing 1 - 3 of 3
  • No Thumbnail Available
    Item
    SDSS IV MaNGA: bar pattern speed in Milky Way analogue galaxies
    (2022) Garma-Oehmichen, L.; Hernandez-Toledo, H.; Aquino-Ortiz, E.; Martinez-Medina, L.; Puerari, I; Cano-Diaz, M.; Valenzuela, O.; Vazquez-Mata, J. A.; Geron, T.; Martinez-Vazquez, L. A.; Lane, R.
    Most secular effects produced by stellar bars strongly depend on the pattern speed. Unfortunately, it is also the most difficult observational parameter to estimate. In this work, we measured the bar pattern speed of 97 Milky-Way analogue galaxies from the MaNGA survey using the Tremaine-Weinberg method. The sample was selected by constraining the stellar mass and morphological type. We improve our measurements by weighting three independent estimates of the disc position angle. To recover the disc rotation curve, we fit a kinematic model to the H alpha velocity maps correcting for the non-circular motions produced by the bar. The complete sample has a smooth distribution of the bar pattern speed (Omega(Bar) = 28.14(-9.55)(+12.30) km s(-1) kpc(-1)), corotation radius (R-CR = 7.82(-2.96)(+3.99) kpc), and the rotation rate (R = 1.35(-0.40)(+0.60)). We found two sets of correlations: (i) between the bar pattern speed, the bar length and the logarithmic stellar mass (ii) between the bar pattern speed, the disc circular velocity and the bar rotation rate. If we constrain our sample by inclination within 30 degrees < i < 60 degrees and relative orientation 20 degrees < vertical bar PA(disc) - PA(bar)vertical bar < 70 degrees, the correlations become stronger and the fraction of ultra-fast bars is reduced from 20 to 10 per cent of the sample. This suggests that a significant fraction of ultra-fast bars in our sample could be associated with the geometric limitations of the TW method. By further constraining the bar size and disc circular velocity, we obtain a subsample of 25 Milky-Way analogues galaxies with distributions Omega(Bar) = 30.48(-6.57)(+10.94) km s(-1) kpc(-1), R-CR = 6.77(-1.91)(+2.32) kpc, and R = 1.45(-0.43)(+0.57) , in good agreement with the current estimations for our Galaxy.
  • No Thumbnail Available
    Item
    SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
    (2022) Cano-Diaz, M.; Hernandez-Toledo, H. M.; Rodriguez-Puebla, A.; Ibarra-Medel, H. J.; Avila-Reese, V; Valenzuela, O.; Medellin-Hurtado, A. E.; Vazquez-Mata, J. A.; Weijmans, A.; Gonzalez, J. J.; Aquino-Ortiz, E.; Martinez-Vazquez, L. A.; Lane, Richard R.
    We present the MaNGA Dwarf galaxy (MaNDala) Value Added Catalog (VAC), from the final release of the Sloan Digital Sky Survey-IV program. MaNDala consists of 136 randomly selected bright dwarf galaxies with M (*) < 10(9.1) M (circle dot) and M ( g ) > -18.5, making it the largest integral field spectroscopy homogeneous sample of dwarf galaxies. We release a photometric analysis of the g, r, and z broadband imaging based on the DESI Legacy Imaging Surveys, as well as a spectroscopic analysis based on the Pipe3D SDSS-IV VAC. Our release includes the surface brightness (SB), geometric parameters, and color profiles, Sersic fits as well as stellar population properties (such as stellar ages, metallicities, and star formation histories), and emission lines' fluxes within the FOV and the effective radii of the galaxies. We find that the majority of the MaNDala galaxies are star-forming late-type galaxies with n (Sersic,r) similar to 1.6 that are centrals (central/satellite dichotomy). MaNDala covers a large range of SB values (we find 11 candidate ultra-diffuse galaxies and three compact ones), filling the gap between classical dwarfs and low-mass galaxies in the Kormendy Diagram and in the size-mass/luminosity relation, which seems to flatten at 10(8) < M (*)/M (circle dot) < 10(9) with R ( e,r ) similar to 2.7 kpc. A large fraction of MaNDala galaxies formed from an early low-metallicity burst of SF, but also from late SF events from more metal-enriched gas: half of the MaNDala galaxies assembled 50% of their mass at z > 2, while the last 20% was at z < 0.3. Finally, a bending of the sSFR-M (*) relation at M (*) similar to 10(9) M (circle dot) for the main-sequence galaxies seems to be supported by MaNDala.
  • No Thumbnail Available
    Item
    Which Galaxy Property is the Best Gauge of the Oxygen Abundance?
    (2022) Alvarez-Hurtado, P.; Barrera-Ballesteros, J. K.; Sanchez, S. F.; Colombo, D.; Lopez-Sanchez, A. R.; Aquino-Ortiz, E.
    We present an extensive exploration of the impact of 29 physical parameters in the oxygen abundance for a sample of 299 star-forming galaxies extracted from the extended Calar Alto Legacy Integral Field Area Survey sample. We corroborate that the stellar mass is the physical parameter that better traces the observed oxygen abundance (i.e., the mass-metallicity relation; MZR), while other physical parameters could play a potential role in shaping this abundance, but with a lower significant impact. We find that the functional form that best describes the MZR is a third-order polynomial function. From the residuals between this best functional form and the MZR, we find that once considered the impact of the mass in the oxygen abundance, the other physical parameters do not play a significant secondary role in shaping the oxygen abundance in these galaxies (including the gas fraction or the star formation rate). Our analysis suggests that the origin of the MZR is related to the chemical enrichment evolution of the interstellar medium due, most likely, to the buildup of stellar mass in these star-forming galaxies.