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Program
| Sunday Feb. 4 | ||
| 16:00 - ... | Registration | |
| 20:30 - 21:30 | Dinner | |
| Monday Feb. 5 | ||
| 9:30 - 10:00 | Welcome, purpose & organization of the meeting | |
| Session I. Chair: Casiana Muñóz-Tuñón | ||
| 10:00 - 10:30 | Itziar Aretxaga | Largest starbursts at z~2 ( PDF 4.18 Mb) |
| 10:30 - 11:00 | Borja Pérez-Díaz | Unveiling chemical enrichment in galaxies through infrared emission lines (
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6.42 Mb) Future and ongoing infrared and radio observatories such as JWST, METIS, and ALMA will increase the amount of rest-frame IR spectroscopic data for galaxies by several orders of magnitude. While studies of the chemical composition of the interstellar medium (ISM) based on optical observations have been widely spread over decades for star-forming galaxies (SFGs) and, more recently, for active galactic nuclei (AGN), similar studies need to be performed using IR data. In the case of AGN, this regime can be especially useful given that it is less affected by temperature and dust extinction, traces higher ionic species, and can also provide robust estimations of the chemical abundance ratio N/O. Moreover, regarding (Ultra)-Luminous Infrared Galaxies ([U]LIRGs), the IR regime peers through their dusty medium and allow us to include the obscured metals in their studies. In this contribution, I will provide a summary of the bayesian-like code HII-CHI-Mistry-IR, which takes advantage of photoionization models, characterized by the chemical abundance ratios O/H and N/O, and the ionization parameter U, to compare their predicted emission-line fluxes with a set of observed values. Instead of matching single emission lines, the code uses some specific emission-line ratios that are sensitive to the above free parameters. I will also review our most recent findings from the study of IR emissions, starting from the performance of the code and its comparison to optical studies, following by a discussion on the universality of the S/O chemical abundance ratio, which can be independently estimate thanks to the set of emission lines available in this regime, and ending up by the finding of deviations from the mass-metallicity relation (MZR) as a consequence of the action of massive inflows of metal poor gas that produces that some galaxies experience a "deep-diving" phase in the MZR diagram as the metals from their ISM are diluted. |
| 11:00 - 11:30 | Pause Caffe | |
| 11:30 - 12:00 | Antonio Arroyo Polonio | Green Pea galaxies seen with MUSE/VLT and HST (
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8.52 Mb) This study offers an in-depth analysis of the kinematic behavior of ionized gas in IZw18, a galaxy notable for its extremely low metallicity and proximity, utilizing data from MEGARA/GTC. We explored the structure and dynamics of the galaxy through H$\alpha$ line profiles, applying single and double Gaussian component fittings to create detailed maps of luminosity, velocity, and velocity dispersion in the main body (MB) and Halo regions of the galaxy. In the MB, a rotational pattern is evident, yet a secondary, more complex kinematic pattern emerges from the double-component fitting, also including a high-energy outflow indicated by a component with a FWHM of 3000 km/s. The NE Halo shows a tranquil state with low velocity dispersions, contrasting the SW Halo presents higher velocities and more complex kinematics. Our findings challenge previous notions of bipolar outflows in IZw18, suggesting instead large-scale turbulent motion. This research enhances our understanding of the dynamics in blue compact dwarf galaxies like IZw18, providing insights into early galaxy formation and the complex kinematics characteristic of such environments. |
| 12:00 - 12:30 | José M. Vílchez | Searching for Extreme Emission Line Galaxies in the miniJPAS and MUSE HUDF surveys (
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7.9 Mb) Authors: José M. Vílchez, Ignacio del Moral- Castro, Jorge Iglesias-Páramo, Antonio Arroyo-Polonio We have performed a deep search for extreme emission line galaxies (EELG) using the miniJPAS survey (Bonoli+ 2021) and the MUSE HUDF survey DR2 (Bacon+ 2023) . This searches have been aimed at extending current samples of EELG and/or Green Pea-like (GP) galaxies towards the lower luminosity domain, including more distant and/or fainter sources. Typically, this family of galaxies are expected to present an extraordinary Lyman continuum photon efficiency for its mass, making them ideal laboratories to study the physical conditions of the potential candidates for the escape of Lyman photons. |
| 12:30 - 13:00 | J. Miguel Mas Hesse | The origin of the leaking ionizing continuum in Haro 11 As the nearest confirmed Lyman continuum (LyC) emitter, Haro 11 is an exceptional laboratory for studying LyC escape processes crucial to cosmic reionization. New HST/COS G130M/1055 observations of its three star-forming knots reveal that the observed LyC originates in Knots B and C. The knot with the strongest LyC detection has the highest LyC production. However, LyC escape is less efficient in Knot B than in Knot C due to higher neutral gas covering. Our results therefore stress the importance of the intrinsic ionizing luminosity, and not just the escape fraction, for LyC detection. Similarly, the Lyα escape fraction does not consistently correlate with LyC flux, nor do narrow Lyα red peaks. High observed Lyα luminosity and low Lyα peak velocity separation, however, do correlate with higher LyC escape. Another insight comes from the undetected Knot A, which drives the Green Pea properties of Haro 11. Its density-bounded conditions suggest highly anisotropic LyC escape. Finally, both of the LyC-leaking Knots, B and C, host ultra-luminous X-ray sources (ULXs). While stars strongly dominate over the ULXs in LyC emission, this intriguing coincidence underscores the importance of unveiling the role of accretors in LyC escape and reionization. |
| 13:00 - 13:30 | Iker Millan Irigoyen | New prospects on HR-pyPopStar evolutionary synthesis models (
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5.21 Mb) |
| 13:30 - 15:00 | Lunch Break | |
| Session II. Chair: Sandra Zamora | ||
| 15:00 - 15:30 | Enrique Pérez Montero | Advances in the study of the softness diagram in the optical and the infrared (
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4.05 Mb) The softness parameter constitutes one of our best tools to explore the hardness of the field of radiation in star-forming galaxies based on the analysis of bright emission-lines. In the last years we have explored its use through is interpretation with large grids of photoionization models and the adaptation of the bayesian code HII-CHI-mistry. The models allow to reduce the dependence of this parameter on metallicity and to separate the derivation of the equivalent effective temperature and the ionization parameter, as well as the inclusion of multiple emission-line ratios measured in the optical and the IR. In this contribution I will summarize some of the results obtained from the analysis of the softness parameter based on optical lines and using models, focusing on the determination of the radial variation of the hardness of the field of radiation in spiral disks, the role of photon leaking on the interpretation of several observed emission-line ratios, or the contamination of outer ionizing sources such as DIG. Finally, I will introduce our results on its equivalent form using fine-structure infrared lines and its use not just for star-forming objects, but also for very powerful sources such as AGNs, discussing how all these brand new strategies can be used to interpret the new available observations taken from the mid-IR, such as with the JWST |
| 15:30 - 16:00 | Jorge Sanchez Almeida | Intermediate mass Black holes and nature of dark matter, and ... (
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8.67 Mb) |
| 16:00 - 16:30 | Salvador Duarte Puertas | Properties of supernova remnants in SIGNALS galaxies - I . NGC 6822 and M 33 There are currently ~1500 known supernova remnants (SNRs) spread across a dozen galaxies where most of them have been identified optically. These objects chemically enrich their host and influence future generations of stars. Distinguishing SNRs from HII regions is not straightforward. Most authors consider an emission lines ratio [SII]/Hα > 0.4 for this. Recently it has been proposed to study the velocity structure to differentiate them as well, since SNRs show a larger velocity broadening than HII regions. In this work we combine these two prescriptions, i.e. the [SII]/Hα value and the velocity structure, for a sample of SNRs in two galaxies of the Local Group, NGC6822 and M33. Both galaxies have been observed with the imaging Fourier transform spectrometer SITELLE (U. Laval and ABB) and installed at the Canada-France-Hawaii Telescope, as part of the SIGNALS survey. Our observations offer a minimum spectral resolution R = 3000. Bearing in mind also the large field of view (11'×11'), high spatial resolution (0.32''/pixel, seeing limited), and the spectral ranges of SITELLE, this work have allowed us to perform a spatially resolved study of all SNR candidates in these two galaxies taking into account these criteria for the first time. From our study we discard some published SNR candidates in NGC6822 and M33. This is the first work in a series dedicated to the detection of all SNRs in the SIGNALS sample. |
| 16:30 - 17:00 | José Miguel Rodríguez Espinosa | A Lyman Alpha Blob at a redshift of 3.5 ( PDF 1.18 Mb) |
| 17:00 - 17:10 | Dedication to José Miguel Rodríguez Espinosa Chair: Casiana Muñóz-Tuñón |
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| 17:10 - 17:30 | Pause Caffe | |
| 17:30 - 18:30 | Discussion: Organizational matters (webpage, outreach, meetings, postdoc calss etc.) Chair: Jorge Sanchez Almeida |
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| 20:30 - 21:30 | Dinner | |
| Tuesday Feb. 6 | ||
| Session III. Chair: J. Miguel Mas Hesse | ||
| 9:30 - 10:00 | Ricardo Amorín | Linking ionized gas kinematics and the escape of ionizing photons in green pea galaxies |
| 10:00 - 10:30 | Maria Luisa Garcia Vargas | MEGASTAR Stellar Library update This short talk gives the update on MEGASTAR project. MEGASTAR is a stellar library being built with spectra at R=20000 taken with MEGARA at the GTC in filler-type time. Two setp-ups are available: one arund Halpha (HR-R) and the other one around CaT (HR-I). the spectra are rectified and the stellar parameters: Teff lgg and [Fe/H] are obtained from comparison with theoretical models. |
| 10:30 - 11:00 | Alejandro Lumbreras Calle | Detecting and following-up extreme emission line galaxies in J-PLUS: connecting the local and early Universe (
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5.95 Mb) Extreme emission line galaxies (EELGs) harbor the strongest unobscured star formation events in the Universe, and they show low gas-phase metallicities, regardless of their redshift. While nearby EELGs are very uncommon, recent JWST results show that typical galaxies at z>6 share many properties with them (intense emission lines, low metallicity and stellar mass, compact morphology, etc.). Low-z EELGs are therefore an ideal laboratory to study in detail the massive star-formation processes occurring in the very early Universe. Given their scarcity, very wide multiband surveys are likely the most efficient tool to uncover large samples of low-z EELG. We use the J-PLUS survey, with photometric observations of 3000 deg2 on the sky with 12 narrow and broadband filters. We have selected over 1000 EELGs at z<0.35 by identifying flux excess in narrowband filters, due to very large equivalent widths (>300 Å) in either the [OIII]5007 or Hα emission lines. Avoiding biases in broadband color selections, we have demonstrated that the number density of this class of objects in the local Universe is roughly 20 times higher than previously reported in photometric studies (Lumbreras-Calle et al. 2022). We have confirmed the selections with spectroscopic follow-up studies. This analysis demonstrates the similarity between our low-z EELGs and JWST-detected galaxies at z>6, e.g. in their position in the mass-metallicity diagram. Further multiwavelength studies of the interstellar medium of low-z EELGs will help us understand the physical properties of star formation in these systems and their reionization-era analogs. |
| 11:00 - 11:30 | Pause Caffe | |
| 11:30 - 12:00 | Roberto Terlevich | Spatially resolved properties of the ionized gas in the H II galaxy J084220+115000 I will present a spectroscopic study of the metal poor H II galaxy J084220+115000 using MEGARA IFU observations at the GTC. Spatially resolved maps indicate that the gas appears to be photoionized by massive stars according to the diagnostic line ratios. The gas metallicity was estimated using the direct method with a mean global value of 12 + log (O/H) = 8.03 ± 0.06, and integrated electron density and temperature of ~160 cm-3 and ~15400 K, respectively. An unusual result in a dwarf star-forming galaxy is that he metallicity distribution shows a large gradient of Δlog(O/H) = 0.72 between the minimum 7.69 ± 0.06 and maximum 8.42 ± 0.05 values. |
| 12:00 - 12:30 | Stefano Zarattini | Fossil groups as isolated structures rather than fossil relics of the ancient Universe (
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5.22 Mb) Fossil groups (FGs) were thought to be the end product of galaxy groups evolution. In this talk we discuss the position of FGs within the cosmic web using a sample of about 70 local cluster and groups, including 15 FGs. We compute their distance to filaments and nodes and show that FGs are found, on average, at larger distances to both filaments and nodes than non-FGs. We thus propose a paradigm shift: FGs are isolated structures rather than fossil relics of the ancient Universe. The formation of the magnitude gap could be linked to internal processes (e.g. infalling galaxies on radial orbits). |
| 12:30 - 13:00 | Asier Castrillo Varona | SNR in PHANGS galaxies, optical properties and their relation with star formation (
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3.04 Mb) We present a new supernova remnant (SNR) catalog for the MUSE-PHANHS survey. This new catalog makes use of machine learning techniques for the unbiased classification of the ionized phase of the ISM, finding more than 480 SNR in our 19 galaxies. We analyze the optical spectral properties of our sample, compare it to state of the art radiative shock models and try to improve the different optical selection criteria to distinguish between HII regions and SNR. In addition, we extract the star formation history (SFH) of the PHANGS galaxies and investigate its relationship with the SNR population using the delay time distribution (DTD) function. |
| 13:00 - 13:30 | Miguel Cerviño | Semi-resolved stellar and Surface Brightness Fluctuations (
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5.60 Mb) Here I address the analysis of stellar populations using surface brightness fluctuations. I show that, although it is usually applied to old stellar populations, it is also applicable to young stellar populations (actually young populations must have a largest signal in SBF analysis). I will show how the method can be applied in several situations, and how it is specially suitable for regimens with a low number of stars per resolution element. |
| 13:30 - 15:00 | Lunch Break | |
| Session IV. Chair: Borja Pérez-Díaz | ||
| 9:00 - 9:30 | Ángeles Díaz Beltrán | Deriving abundance gradients across galaxy discs (
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8.40 Mb) The methods to derive abundance gradients across the full extent of discs in spiral galaxies in the different metallicity regimes are reviewed. |
| 9:00 - 9:30 | Casiana Muñóz-Tuñón | The PAU survey: classifying low-z SEDs using Machine Learning clustering |
| 9:00 - 9:30 | Jorge Iglesias Páramo | TARSIS & MOSAIC:new instrumentation in Estallidos8 |
| 16:30 - 17:00 | Pause Caffe | |
| 17:00 - 18:00 | Discussion: Joint project for Esatllidos 8 Chair: José M. Vílchez |
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| 20:30 - 21:30 | Dinner | |
| Wednesday Feb. 7 | ||
| Session V. Chair: Miguel Cerviño | ||
| 9:30 - 10:30 | Sandra Zamora | Star formation processes in the circumnuclear environment of galaxies The inner zones of some galaxies show star formation rates higher than the average observed in galactic discs, frequently arranged in ring structures with a diameter of about 1kpc, named circumnuclear starforming regions (CNSFR). They are commonly referred to as ‘hotspots’ and they appear in early spiral galaxies, many of them showing bars, with or without an active nucleus. They are a common mode of star formation showing similar and large luminosities of disk HII regions but look more compact and show higher peak surface brightness. Due to their specific locations, these regions constitute excellent places to study how star formation proceeds in high metallicity and high density environments. Hence, the main goal of this project is to understand the star formation processes in the young stellar clusters powering CNSFRs using optical integral field spectroscopy observations from MUSE (Multi Unit Spectroscopic Explorer) and MEGARA (Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía). Thus, the principal aim of this work is to investigate the origin of the nuclear emission and its connection with the star formation processes which are taking place in this hostile environment through a simultaneous analysis of the ionized gas and the stellar emission. |
| 10:00 - 10:30 | Elena Terlevich | TBD |
| 10:30 - 11:00 | Bruce Elmegreen | Estallidos 8, WS XIV "Extreme Star Formation" (
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3.18 Mb) |
| 11:00 - 11:30 | Daniel Reverte Payá | Mejoras de Operación e impacto en la comunidad Se mostrarán las mejoras proyectadas en operación científica, y lo que esperamos sea de impacto positivo en la comunidad científica. |
| 11:30 - 12:00 | Pause Caffe | |
| 12:00 - 13:00 | Discussion: Grand conclusions & closing remarks Chair: Ángeles Díaz |
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| 13:30 - 15:00 | Lunch & leaving | |
Goto: [ Top ] [ Program ] [ Participants ]
Participants
| Ricardo Amorín (CEFCA) | Antonio Giménez Alcázar (IAA) | Enrique Pérez Montero (IAA-CSIC) |
| Itziar Aretxaga (INAOE) | Carlos Hoyos (UAM)) | Daniel Reverte Payá (GRANTECAN) |
| Antonio Arroyo Polonio (IAA-CSIC) | Jorge Iglesias Páramo (IAA) | José Miguel Rodríguez Espinosa (IAA) |
| Juanjo Bazán (UAM) | Carolina Kehrig (IAA-CSIC) | Jorge Sanchez Almeida (IAC) |
| Asier Castrillo Varona (UAM) | Alejandro Lumbreras Calle (CEFCA) | Maria Santos Lleó (ESA) |
| Miguel Cerviño (CAB (CSIC-INTA)) | J. Miguel Mas Hesse (CAB (CSIC-INTA)) | Elena Terlevich (INAOE) |
| Angeles Diaz Beltrán (UAM) | Iker Millan Irigoyen (MPA) | Roberto Terlevich (INAOE & IoA) |
| Salvador Duarte Puertas (UGR) | Juan Antonio Molina Calzada (UCM, CAB) | José M. Vílchez (IAA-CSIC) |
| Bruce Elmegreen | Mercedes Mollá (CIEMAT) | Sandra Zamora (UAM) |
| Mata G. (UAM) | Casiana Muñoz Tuñon (IAC) | Stefano Zarattini (IAC) |
| Maria Luisa Garcia Vargas (FRACTAL S.L.N.E.) | Borja Pérez-Díaz (IAA-CSIC) |