Start year
1986
Organizational Unit
Organizing institutions
Grants related:
General
Description
The basic objective of the broject is to investigate the evolution of galaxies by deepening our understanding of the interaction between the insterstellar medium and the stars.The main technique which we use is the two-dimensional kinematic study of whole galaxies observed using our instrument:GHaFaS, a Fabry-Perot interferometer on the William Herschel Telescope of the ORM.
We combine the data from GHaFaS with our own photometric imaging using ACAM on the same telescope, with a variety of sources of images in the infrared and ultraviolet, and with emission line maps en the radio and milimetre range to explore the effects, and the physical parameters which the determine the star formation rate and the mass function of the stars depending on the sites of their formation in galaxies.
In the present phase of the project the dynamical aspects which we are e xploring are basically two: the resonant structure of discs and bars, and the effects of the zones of massive star formation on their surroundings via stellar winds and supernovae.In addition, in preparation for the exploration of galaxy formation in earlier epochs, we are studying how the interactions between galaxies stimulate and condition star formation within them before they merge. In the future these studies will be extended, methodically, in two directions: outwards to galaxies at increasing redshift, and inwards by applying our methods to the study of interstellar porcesse in the zones of massive star formation in the Local Group galaxy M33.
We combine our research into galaxy kinematics with evolutionary aspects of galaxy discs based on precise observations of their surface brightness profiles, both in local galaxies and in galaxies at intermediate redshift. In order to make progress in this direction we are collaborating with colleagues at the Instituto de Astronomía de la UNAM (México) and the Laboratoire d'Astrophysique de Marseille (France) in the implementation of a new instrument, NEFER, which will be a high resolution Fabry-Perot module incorporated into OSIRIS on the GTC. We had successful inicial trials in December 2017, and commissioneed NEFER in March 2018 for use as a visitor instrument permanently on the GTC.
Members
Principal investigator
Prof.
John E. Beckman
Project staff
Dr.
J. Font
Collaborators
Dr.
M. Rosado
Dr.
A. Rodríguez
Dr.
P. Velázquez
Dr.
A. Camps
Dr.
L. Gutierrez Albores
Dr.
P. Amram
Dr.
S. Comerón
Dr.
B. Epinat
María Begoña
García Lorenzo
Johan Hendrik
Knapen Koelstra
Ignacio
Trujillo Cabrera
Results
- The "Font-Beckman" method for analysing resonances in galaxies was shown to give very accurate results, comparing it with the "Tremaine-Weinberg" method using data from GHaFaS (WHT and MUSE (VLT)
- The profiles of Type III (antitruncated) S0 galaxies were measured at z = 0.6 (5 thousan dmillion years ago) for the first time. The "break radius" is the same as that of local galaxies, but its surface brightness is 1.6 magnitudes brighter.
- A new and greatly improved analysis of the Hubble Ultra-Deep Field gave an image with valid photometry down to 33 mag /arcsec squared, revealing the faint outskirts of it galaxies,.
- Comparing galaxies in interacting pairs with isolated galaxies it was shown that the star formation rate in the former is consistently enhanced and that this enhancement is common to the discs and the tidal tails
- The galaxy NGC 864 (CIG 86), apparently isolated, shows an asymmetric distribution of its hI. It was shown that this galaxy is truly isolated, and that HI accretion probably accounts for the asymmetry as well as the star formation in its stellar pseud-ring
Scientific activity
Related publications
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A quantitative demonstration that stellar feedback locally regulates galaxy growthWe have applied stellar population synthesis to 500-pc-sized regions in a sample of 102 galaxy discs observed with the MUSE spectrograph. We derived the star formation history and analyse specifically the 'recent' ( $20\,\rm {Myr}$ ) and 'past' ( $570\,\rm {Myr}$ ) age bins. Using a star formation self-regulator model, we can derive local massZaragoza-Cardiel, Javier et al.
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92020 -
Arp 70: an interacting galaxy with extreme outflowsWe analysed a Fabry-Pérot (FP) cube of the interacting pair of galaxies Arp 70, which was obtained from the CeSAM public repository of FP data. On the larger galaxy Arp 70b, we detected the spectral signature of two different outflows, one located in the centre and the other associated with a giant H II region in the arm region. The central outflowCamps-Fariña, A. et al.
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32020 -
Detection of the self-regulation of star formation in galaxy discsStellar feedback has a notable influence on the formation and evolution of galaxies. However, direct observational evidence is scarce. We have performed stellar population analysis using MUSE optical spectra of the spiral galaxy NGC 628 and find that current maximum star formation in spatially resolved regions is regulated according to the level ofZaragoza-Cardiel, Javier et al.
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62019 -
The missing light of the Hubble Ultra Deep FieldContext. The Hubble Ultra Deep field (HUDF) is the deepest region ever observed with the Hubble Space Telescope. With the main objective of unveiling the nature of galaxies up to z ˜ 7 - 8, the observing and reduction strategy have focused on the properties of small and unresolved objects, rather than the outskirts of the largest objects, which areBorlaff, A. et al.
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12019 -
Spiral structure in barred galaxies. Observational constraints to spiral arm formation mechanismsA method, which we have developed for determining corotation radii, has allowed us to map in detail the radial resonant structures of barred spiral galaxies. Here, we have combined this information with new determinations of the bar strength and the pitch angle of the innermost segment of the spiral arms to find relationships between theseFont, J. et al.
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22019 -
Unveiling the environment and faint features of the isolated galaxy CIG 96 with deep optical and HI observationsContext. Asymmetries in atomic hydrogen (HI) in galaxies are often caused by the interaction with close companions, making isolated galaxies an ideal framework to study secular evolution. The AMIGA project has demonstrated that isolated galaxies show the lowest level of asymmetry in their HI integrated profiles compared to even field galaxies, yetRamírez-Moreta, P. et al.
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112018 -
Formation of S0 galaxies through mergers. Morphological properties: tidal relics, lenses, ovals, and other inner componentsContext. Major mergers are popularly considered too destructive to produce the relaxed regular structures and the morphological inner components (ICs) usually observed in lenticular (S0) galaxies. Aims: We aim to test if major mergers can produce remnants with realistic S0 morphologies. Methods: We have selected a sample of relaxed discy remnantsEliche-Moral, M. C. et al.
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102018 -
Evolution of the anti-truncated stellar profiles of S0 galaxies since z = 0.6 in the SHARDS survey. II. Structural and photometric evolutionContext. Anti-truncated lenticular galaxies (Type-III S0s) present tight scaling relations between their surface brightness photometric and structural parameters. Although several evolutionary models have been proposed for the formation of these structures, the observations of Type-III S0 galaxies are usually limited to the local Universe. Aims: WeBorlaff, A. et al.
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72018 -
Precision Determination of Corotation Radii in Galaxy Disks: Tremaine–Weinberg versus Font–Beckman for NGC 3433Density waves in galaxy disks have been proposed over the years, in a variety of specific models, to explain spiral arm structure and its relation to the mass distribution, notably in barred galaxies. An important parameter in dynamical density wave theories is the corotation radius, the galactocentric distance at which the stars and gas rotate atBeckman, J. E. et al.
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22018 -
Stellar Population Synthesis of Star-forming Clumps in Galaxy Pairs and Non-interacting Spiral GalaxiesWe have identified 1027 star-forming complexes in a sample of 46 galaxies from the Spirals, Bridges, and Tails (SB&T) sample of interacting galaxies, and 693 star-forming complexes in a sample of 38 non-interacting spiral (NIS) galaxies in 8 μm observations from the Spitzer Infrared Array Camera. We have used archival multi-wavelength UV-to IRZaragoza-Cardiel, J. et al.
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22018 -
280 one-opposition near-Earth asteroids recovered by the EURONEAR with the Isaac Newton TelescopeContext. One-opposition near-Earth asteroids (NEAs) are growing in number, and they must be recovered to prevent loss and mismatch risk, and to improve their orbits, as they are likely to be too faint for detection in shallow surveys at future apparitions. Aims: We aimed to recover more than half of the one-opposition NEAs recommended forVaduvescu, O. et al.
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12018 -
The ALHAMBRA survey: 2D analysis of the stellar populations in massive early-type galaxies at z < 0.3We present a technique that permits the analysis of stellar population gradients in a relatively low-cost way compared to integral field unit (IFU) surveys. We developed a technique to analyze unresolved stellar populations of spatially resolved galaxies based on photometric multi-filter surveys. This technique allows the analysis of vastly largerSan Roman, I. et al.
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12018 -
Formation of S0 galaxies through mergers. Evolution in the Tully-Fisher relation since z ∼ 1Context. Lenticular (S0) galaxies are known to derive from spiral galaxies. The fact that S0s nearly obey the Tully-Fisher relation (TFR) at z ∼ 0 (as spirals have done in the last 9 Gyr) is considered an argument against their major-merger origin because equal mergers of two disc galaxies produce remnants that are outliers of the TFR. Aims: WeTapia, T. et al.
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82017 -
Evolution of the anti-truncated stellar profiles of S0 galaxies since z = 0.6 in the SHARDS survey. I. Sample and methodsContext. The controversy about the origin of the structure of early-type S0-E/S0 galaxies may be due to the difficulty of comparing surface brightness profiles with different depths, photometric corrections and point spread function (PSF) effects (which are almost always ignored). Aims: We aim to quantify the properties of Type-III (anti-truncated)Borlaff, A. et al.
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82017 -
Balmer Filaments in Tycho’s Supernova Remnant: An Interplay between Cosmic-ray and Broad-neutral PrecursorsWe present Hα spectroscopic observations and detailed modeling of the Balmer filaments in the supernova remnant (SNR) Tycho (SN 1572). We used GH α FaS (Galaxy Hα Fabry–Pérot Spectrometer) on the William Herschel Telescope with a 3.‧4 × 3.‧4 field of view, 0.″2 pixel scale, and {σ }{instr}=8.1 km s‑1 resolution at 1″ seeing for ∼10 hr, resulting inKnežević, S. et al.
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92017 -
Physical properties of superbubbles in the Antennae galaxiesMass outflow generated by the dynamical feedback from massive stars is currently a topic of great interest. Using a purpose-developed analysis technique, and taking full advantage of the high kinematic and angular resolution of our instrument, we have detected a number of expanding superbubbles in the interacting pair of galaxies Arp 244 (NGC 4038Rosado, M. et al.
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72017 -
The molecular gas mass of M 33Do some environments favor efficient conversion of molecular gas into stars? To answer this, we need to be able to estimate the H2 mass. Traditionally, this is done using CO observations and a few assumptions but the Herschel observations which cover the far-IR dust spectrum make it possible to estimate the molecular gas mass independently of COGratier, P. et al.
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32017 -
Kinematics of the ionized and molecular gas in nearby luminous infrared interacting galaxiesWe have observed three luminous infrared galaxy systems which are pairs of interacting galaxies, with the Galaxy Hα Fabry-Perot system mounted on the 4.2 m William Herschel Telescope at the Roque de los Muchachos Observatory, and combined the observations with the Atacama Large Millimeter Array observations of these systems in CO emission toZaragoza-Cardiel, J. et al.
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32017 -
Kinematic Clues to Bar Evolution for Galaxies in the Local Universe: Why the Fastest Rotating Bars are Rotating Most SlowlyWe have used Spitzer images of a sample of 68 barred spiral galaxies in the local universe to make systematic measurements of bar length and bar strength. We combine these with precise determinations of the corotation radii associated with the bars, taken from our previous study, which used the phase change from radial inflow to radial outflow ofFont, J. et al.
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22017 -
The UK Infrared Telescope M 33 monitoring project - V. The star formation history across the galactic discWe have conducted a near-infrared monitoring campaign at the UK Infrared Telescope of the Local Group spiral galaxy M 33 (Triangulum). On the basis of their variability, we have identified stars in the very final stage of their evolution, and for which the luminosity is more directly related to the birth mass than the more numerous less-evolvedJavadi, A. et al.
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12017
