J. P. Nogueira-Cavalcante

National Observatory

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I. Araya

Universidad Mayor

Karín Menéndez‐Delmestre

Valongo Observatory

A. Shokry

National Research Institute of Astronomy and Geophysics

L. Saker

Argentine National Observatory

B. Dias

Universidad Andrés Bello

Thiago S. Gonçalves

Universidade Federal do Rio de Janeiro

P. Sánchez–Blázquez

Universidad Complutense de Madrid

J. Varela

Centro de Estudios de Física del Cosmos de Aragón

Ana L. Chies-Santos

Universidade Federal do Rio Grande do Sul

D. Cristòbal-Hornillos

Centro de Estudios de Física del Cosmos de Aragón

Cooperative Institutions

Centro de Estudios de Física del Cosmos de Aragón

Valongo Observatory

Universidade de São Paulo

Instituto de Astrofísica de Canarias

Consejo Superior de Investigaciones Científicas

Universidad de La Laguna

National Observatory

Museu de Astronomia e Ciências Afins

Instituto de Astrofísica de Andalucía

Laboratório Nacional de Astrofísica

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Measuring quenching timescales in green valley galaxies

IAUGA (2015)

Thiago S. Gonçalves Christopher Martin J. P. Nogueira-Cavalcante Karín Menéndez‐Delmestre Kartik Sheth

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Galactic or extragalactic chemical tagging for NGC 3201?

Astronomy and Astrophysics (2018)

B. Dias I. Araya J. P. Nogueira-Cavalcante L. Saker A. Shokry

(ABRIDGED) The origin of the globular cluster (GC) NGC3201 is under debate. Its retrograde orbit points to an extragalactic origin, but no further chemical evidence supports this idea. Light-element chemical abundances are useful to tag GCs and can be used to shed light on this discussion. We aim to derive CN and CH band strengths for red giant stars in NGC3201 and compare these with photometric indices and high-resolution spectroscopy and discuss in the context of GC chemical tagging. We found three groups in the CN-CH distribution. A main sequence (S1), a secondary less-populated sequence (S2), and a group of peculiar (pec) CN-weak and CH-weak stars, one of which was previously known. The three groups seem to have different C+N+O and/or s-process element abundances, to be confirmed by high-resolution spectroscopy. These are typical characteristics of anomalous GCs. The CN distribution of NGC 3201 is quadrimodal, which is more common in anomalous clusters. However, NGC3201 does not belong to the trend of anomalous GCs in the mass-size relation. Three scenarios are postulated here: (i) if the sequence pec-S1-S2 has increasing C+N+O and s-process element abundances, NGC3201 would be the first anomalous GC outside of the mass-size relation; (ii) if the abundances are almost constant, NGC3201 would be the first non-anomalous GC with multiple CN-CH anti-correlation groups; or (iii) it would be the first anomalous GC without variations in C+N+O and s-process element abundances. In all cases, the definition of anomalous clusters and the scenario in which they have an extragalactic origin must be revised.

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10.1051/0004-6361/201731957

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J-PLUS: The Javalambre Photometric Local Universe Survey

Astronomy and Astrophysics (2018)

A. J. Cenarro M. Moles D. Cristòbal-Hornillos A. Marín-Franch A. Ederoclite

J-PLUS is an ongoing 12-band photometric optical survey, observing thousands of square degrees of the Northern hemisphere from the dedicated JAST/T80 telescope at the Observatorio Astrof\'isico de Javalambre. T80Cam is a 2 sq.deg field-of-view camera mounted on this 83cm-diameter telescope, and is equipped with a unique system of filters spanning the entire optical range. This filter system is a combination of broad, medium and narrow-band filters, optimally designed to extract the rest-frame spectral features (the 3700-4000\AA\ Balmer break region, H$\delta$, Ca H+K, the G-band, the Mgb and Ca triplets) that are key to both characterize stellar types and to deliver a low-resolution photo-spectrum for each pixel of the sky observed. With a typical depth of AB $\sim 21.25$ mag per band, this filter set thus allows for an indiscriminate and accurate characterization of the stellar population in our Galaxy, it provides an unprecedented 2D photo-spectral information for all resolved galaxies in the local universe, as well as accurate photo-z estimates ($\Delta\,z\sim 0.01-0.03$) for moderately bright (up to $r\sim 20$ mag) extragalactic sources. While some narrow band filters are designed for the study of particular emission features ([OII]/$\lambda$3727, H$\alpha$/$\lambda$6563) up to $z < 0.015$, they also provide well-defined windows for the analysis of other emission lines at higher redshifts. As a result, J-PLUS has the potential to contribute to a wide range of fields in Astrophysics, both in the nearby universe (Milky Way, 2D IFU-like studies, stellar populations of nearby and moderate redshift galaxies, clusters of galaxies) and at high redshifts (ELGs at $z\approx 0.77, 2.2$ and $4.4$, QSOs, etc). With this paper, we release $\sim 36$ sq.deg of J-PLUS data, containing about $1.5\times 10^5$ stars and $10^5$ galaxies at $r<21$ mag.

Balmer series

Spectral resolution

Stellar population

10.1051/0004-6361/201833036

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J-PLUS: Impact of bars on quenching timescales in nearby green valley disc galaxies

Astronomy and Astrophysics (2019)

J. P. Nogueira-Cavalcante Renato A. Dupke P. Coelho M. L. L. Dantas Thiago S. Gonçalves

In a framework where galaxies mostly migrate on the colour-magnitude diagram from star-forming to quiescent, the green valley is considered a transitional galaxy stage. The details of the processes that drive galaxies from star-forming to passive systems still remain unknown. We developed a method that estimates empirically the star formation quenching times-scales of green valley galaxies, assuming an exponential decay model of the SFH and through a combination of narrow and broad bands from J-PLUS and GALEX. We correlate these quenching time-scales with the presence of bars. We find that the J-PLUS colours F0395-g and F0415-g are sensitive to different SFH, showing, a clear correlation with the Dn(4000) and H-delta,A spectral indices. We find that quenching time-scales obtained with our new approach are in agreement with those determined using spectral indices. We also find that galaxies with high bar probability tend to quench their star formation slowly. We conclude that: 1) J-PLUS filters can be used to measure quenching timescales in nearby green valley galaxies; and 2) the resulting star formation quenching time-scales are longer for barred green valley galaxies. Considering that the presence of a bar indicates that more violent processes (e.g., major mergers) are absent in host galaxies, we conclude that the presence of a bar can be used as a morphological signature for slow star formation quenching.

10.1051/0004-6361/201935138

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Galactic or extragalactic chemical tagging for NGC 3201?: Discovery of an anomalous CN-CH relation

B. Dias I. Araya J. P. Nogueira-Cavalcante L. Saker A. Shokry

Context. The origin of the globular cluster (GC) NGC 3201 is under debate. Its retrograde orbit points to an extragalactic origin, but no further chemical evidence supports this idea. Light-element chemical abundances are useful to tag GCs and can be used to shed light on this discussion.Aims. Recently it was shown that the CN and CH indices are useful to identify GCs that are anomalous to those typically found in the Milky Way. A possible origin of anomalous clusters is the merger of two GCs and/or the nucleus of a dwarf galaxy. We aim to derive CN and CH band strengths for red giant stars in NGC3201 and compare these with photometric indices and high-resolution spectroscopy and discuss in the context of GC chemical tagging.Methods. We measure molecular band indices of S(3839) and G4300 for CN and CH, respectively from low-resolution spectra of red giant stars. Gravity and temperature effects are removed. Photometric indices are used to indicate further chemical information on C+N+O or s -process element abundances that are not derived from low-resolution spectra.Results. We found three groups in the CN–CH distribution. A main sequence (S1 ), a secondary less-populated sequence (S2 ), and a group of peculiar (pec ) CN-weak and CH-weak stars, one of which was previously known. The three groups seem to have different C+N+O and/or s -process element abundances, to be confirmed by high-resolution spectroscopy. These are typical characteristics of anomalous GCs. The CN distribution of NGC 3201 is quadrimodal, which is more common in anomalous clusters. However, NGC 3201 does not belong to the trend of anomalous GCs in the mass-size relation.Conclusions. The globular cluster NGC 3201 shows signs that it can be chemically tagged as anomalous: it has an unusual CN–CH relation, indications that pec -S1 -S2 is an increasing sequence of C+N+O or s -process element abundances, and a multi-modal CN distribution that seems to correlate with s -process element abundances. The non-anomalous characteristics are that it has a debatable Fe-spread and it does not follow the trend of mass size of all anomalous clusters. Three scenarios are postulated here: (i) if the sequence pec-S1-S2 has increasing C+N+O and s -process element abundances, NGC 3201 would be the first anomalous GC outside of the mass-size relation; (ii) if the abundances are almost constant, NGC 3201 would be the first non-anomalous GC with multiple CN–CH anti-correlation groups; or (iii) it would be the first anomalous GC without variations in C+N+O and s -process element abundances. In all cases, the definition of anomalous clusters and the scenario in which they have an extragalactic origin must be revised.

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VizieR Online Data Catalog: Stellar parameters of NGC3201 RGB stars (Dias+, 2018)

VizieR Online Data Catalog (2018)

B. Dias I. Araya J. P. Nogueira-Cavalcante L. Saker A. Shokry

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Galactic or extragalactic chemical tagging for NGC3201? Discovery of an anomalous CN-CH relation

arXiv (Cornell University) (2018)

B. Dias I. Araya J. P. Nogueira-Cavalcante L. Saker A. Shokry

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J-PLUS: Two-dimensional analysis of the stellar population in NGC 5473 and NGC 5485

Astronomy and Astrophysics (2019)

I. San Roman P. Sánchez–Blázquez A. J. Cenarro L. A. Díaz-García C. López-Sanjuán

The spatial variations of stellar population properties within a galaxy are intimately related to their formation process. Therefore, spatially resolved studies of galaxies are essential to uncover their formation and assembly. The Javalambre Photometric Local Universe Survey (J-PLUS) is a dedicated multi-filter designed to observed ~8500 deg2 using twelve narrow-, intermediate- and broad-band filters in the optical range. In this study, we test the potential of the multi-filter observation carried out with J-PLUS to investigate the properties of spatially-resolved nearby galaxies. We present detailed 2D maps of stellar population properties (age, metallicity, extinction, and stellar mass surface density) for two early-type galaxies observed in both, J-PLUS and CALIFA surveys: NGC 5473 and NGC 5485. Radial structures are also compared and luminosity- and mass-weighted profiles are derived. We use MUFFIT to process the J-PLUS observations, and two different techniques (STARLIGHT and STECKMAP) to analyze IFU CALIFA data. We demonstrate that this novel technique delivers radial stellar population gradients in good agreement with the IFU technique CALIFA/STECKMAP although comparison of the absolute values reveals the existence of intrinsic systematic differences. Radial stellar population gradients differ when CALIFA/STARLIGHT methodology is used. Age and metallicity radial profiles derived from J-PLUS/MUFFIT are very similar when luminosity- or mass-weighted properties are used, suggesting that the contribution of a younger component is small. Comparison between the three methodologies reveals some discrepancies suggesting that the specific characteristics of each method causes important differences. We conclude that the ages, metallicities and extinction derived for individual galaxies not only depend on the chosen models but also depend on the method used.

Stellar population

Stellar mass

Starlight

Extinction (optical mineralogy)

10.1051/0004-6361/201832894

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Compact Galaxies at intermediate redshifts quench faster than normal-sized Galaxies

Monthly Notices of the Royal Astronomical Society (2019)

J. P. Nogueira-Cavalcante Thiago S. Gonçalves Karín Menéndez‐Delmestre I. G. de la Rosa A. Charbonnier

Massive quiescent compact galaxies have been discovered at high redshifts, associated with rapid compaction and cessation of star formation (SF). In this work, we set out to quantify the time-scales in which SF is quenched in compact galaxies at intermediate redshifts. For this, we select a sample of green valley galaxies within the COSMOS field in the midst of quenching their SF at 0.5 < |$z$| < 1.0 that exhibit varying degrees of compactness. Based on the Hδ absorption line and the 4000 Å break of coadded zCOSMOS spectra for subsamples of normal-sized and compact galaxies we determine quenching time-scales as a function of compactness. We find that the SF quenching time-scales in green valley compact galaxies are much shorter than in normal-sized ones. In an effort to understand this trend, we use the Illustris simulation to trace the evolution of the SF history, the growth rate of the central super massive black hole (SMBH), and the AGN feedback in compact and normal-sized galaxies. We find that the difference in SF quenching time-scales is due to the mode of the AGN feedback. In the compact galaxies the kinematic-mode is dominant, being highly efficient at quenching the SF by depleting the internal gas. For normal-sized galaxies, the prevailing thermal-mode injects energy into the circumgalactic gas, preventing cold gas accretion and quenching SF via the slower strangulation mechanism. These results are consistent with the violent disc instability and gas-rich mergers scenarios, followed by strong AGN and stellar feedback. Although this kind of event is most expected to occur at |$z$| = 2–3, we find evidences that the formation of compact quiescent galaxies can occur at |$z$| < 1.

10.1093/mnras/stz190

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The angular scale of homogeneity in the local Universe with the SDSS blue galaxies

Monthly Notices of the Royal Astronomical Society (2019)

Felipe Avila Camila P. Novaes Armando Bernui Edilson de Carvalho J. P. Nogueira-Cavalcante

We probe the angular scale of homogeneity in the local Universe using blue galaxies from the SDSS survey as a cosmological tracer. Through the scaled counts in spherical caps, $ \mathcal{N}(<\theta) $, and the fractal correlation dimension, $\mathcal{D}_{2}(\theta)$, we find an angular scale of transition to homogeneity for this sample of $\theta_{\text{H}} = 22.19^{\circ} \pm 1.02^{\circ}$. A comparison of this measurement with another obtained using a different cosmic tracer at a similar redshift range ($z < 0.06$), namely, the HI extragalactic sources from the ALFALFA catalogue, confirms that both results are in excellent agreement (taking into account the corresponding bias correction). We also perform tests to asses the robustness of our results. For instance, we test if the size of the surveyed area is large enough to identify the transition scale we search for, and also we investigate a reduced sample of blue galaxies, obtaining in both cases a similar angular scale for the transition to homogeneity. Our results, besides confirming the existence of an angular scale of transition to homogeneity in different cosmic tracers present in the local Universe, show that the observed angular scale $\theta_{\text{H}}$ agrees well with what is expected in the $\Lambda$CDM scenario. Although we can not prove spatial homogeneity within the approach followed, our results provide one more evidence of it, strengthening the validity of the Cosmological Principle.

Angular diameter

Observational cosmology

10.1093/mnras/stz1765

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Citations (27)