Examinando por Autor "Saito R.K."

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    Assessing the photometric redshift precision of the S-PLUS survey: The Stripe-82 as a test-case
    (Oxford University Press, 2020-12) Molino A.; Costa-Duarte M.V.; Sampedro L.; Herpich F.R.; Sodré L.; Jr. Mendes de Oliveira C.; Schoenell W.; Barbosa C.E.; Queiroz C.; Lima E.V.R.; Azanha L.; Muñoz-Elgueta N.; Ribeiro T.; Kanaan A.; Hernandez-Jimenez J.A.; Cortesi A.; Akras S.; Lopes de Oliveira R.; Torres-Flores S.; Lima-Dias C.; Nilo Castellon J.L.; Damke G.; Alvarez-Candal A.; Jiménez-Teja Y.; Coelho P.; Pereira E.; Montero-Dorta A.D.; Benítez N.; Gonçalves T.S.; Santana-Silva L.; Werner S.V.; Almeida L.A.; Lopes P.A.A.; Chies-Santos A.L.; Telles E.; Thom de Souza R.C.; Gonçalves D.R.; de Souza R.S.; Makler M.; Buzzo M.L.; Placco V.M.; Nakazono L.M.I.; Saito R.K.; Overzier R.A.; Abramo L.R.
    In this paper we present a thorough discussion about the photometric redshift (photo-z) performance of the Southern Photometric Local Universe Survey (S-PLUS). This survey combines a seven narrow +5 broad passband filter system, with a typical photometric-depth of r ∼ 21 AB. For this exercise, we utilize the Data Release 1 (DR1), corresponding to 336 deg2 from the Stripe-82 region. We rely on the BPZ2 code to compute our estimates, using a new library of SED models, which includes additional templates for quiescent galaxies. When compared to a spectroscopic redshift control sample of ∼100 k galaxies, we find a precision of σz <0.8 per cent, <2.0 per cent, or <3.0 per cent for galaxies with magnitudes r < 17, <19, and <21, respectively. A precision of 0.6 per cent is attained for galaxies with the highest Odds values. These estimates have a negligible bias and a fraction of catastrophic outliers inferior to 1 per cent. We identify a redshift window (i.e. 0.26 < z < 0.32) where our estimates double their precision, due to the simultaneous detection of two emission lines in two distinct narrow bands; representing a window opportunity to conduct statistical studies such as luminosity functions. We forecast a total of ∼2 M, ∼16 M and ∼32 M galaxies in the S-PLUS survey with a photo-z precision of σz <1.0 per cent, <2.0 per cent, and <2.5 per cent after observing 8000 deg2. We also derive redshift probability density functions, proving their reliability encoding redshift uncertainties and their potential recovering the n(z) of galaxies at z < 0.4, with an unprecedented precision for a photometric survey in the Southern hemisphere. © 2020 The Author(s)
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    Ítem
    Discovery of a mid-infrared protostellar outburst of exceptional amplitude
    (Oxford University Press, 2020-12) Lucas P.W.; Elias J.; Points S.; Guo Z.; Smith L.C.; Stecklum B.; Vorobyov E.; Morris C.; Borissova J.; Kurtev R.; Contreras Peña C.; Medina N.; Minniti D.; Ivanov V.D.; Saito R.K.
    We report the discovery of a mid-infrared outburst in a young stellar object (YSO) with an amplitude close to 8 mag at λ ≈ 4.6 μm. WISEA J142238.82-611553.7 is one of 23 highly variable Wide-field Infrared Survey Explorer (WISE) sources discovered in a search of infrared dark clouds (IRDCs). It lies within the small IRDC G313.671-0.309 (d ≈ 2.6 kpc), seen by the Herschel/Hi-Gal survey as a compact massive cloud core that may have been measurably warmed by the event. Pre-outburst data from Spitzer in 2004 suggest it is a class I YSO, a view supported by observation of weak 2.12 μm H2 emission in an otherwise featureless red continuum spectrum in 2019 (6 mag below the peak in Ks). Spitzer, WISE, and VISTA Variables in the Via Lactea (VVV) data show that the outburst began by 2006 and has a duration >13 yr, with a fairly flat peak from 2010 to 2014. The low pre-outburst luminosity implies a low-mass progenitor. The outburst luminosity of a few × 102 L⊙ is consistent with an accretion rate M ≈ 10-4 M⊙yr-1, comparable to a classical FU Orionis event. The 4.6 μm peak in 2010 implies T = 800-1000 K and a disc radial location R ≈ 4.5 au for the emitting region. The colour evolution suggests subsequent progression outwards. The apparent absence of the hotter matter expected in thermal instability or MRI models may be due to complete obscuration of the innermost disc, e.g. by an edge-on disc view. Alternatively, disc fragmentation/infalling fragment models might more naturally explain a mid-infrared peak, though this is not yet clear. © 2020 The Author(s).
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    Ítem
    VVVX survey dusts off a new intermediate-age star cluster in the Milky Way disk
    (EDP Sciences, 2024-08) Garro E.R.; Minniti D.; Alonso-García J.; Fernández-Trincado J.G.; Gómez M.; Palma T.; Saito R.K.; Obasi C.
    Context. In the last decade, many new star clusters have been discovered in heavily obscured regions of the Milky Way bulge and disk. Aims. Our primary long-term objective is to seek out additional star clusters in the poorly studied regions of the Milky Way, where detections pose significant challenges. The aim of this pursuit is to finalize the Milky Way's globular and open cluster system census and to gain a comprehensive understanding of both the formation and evolution of these systems and our Galaxy as a whole. Methods. We report the discovery of a new star cluster, named Garro 03. We investigated this new target using a combination of near-infrared and optical databases. We employed the VISTA Variables in the Via Láctea Survey and Two Micron All Sky Survey data in the near-infrared, and the Gaia Data Release 3 and the DECam Plane Survey datasets in the optical passband. We constructed density maps and vector proper motion diagrams in order to highlight our target. We performed a photometrical analysis in order to derive its main physical parameters. Results. Garro 03 is located at equatorial coordinates RA = 14:01:29.3 and Dec = -65:30:57.0. From our photometric analysis we find that this cluster is not heavily affected by extinction with AKs = 0.25 ± 0.04 mag and AG = 1.54 ± 0.02 mag. It is located at heliocentric distance of 14.1 ± 0.5 kpc, which places Garro 03 at 10.6 kpc from the Galactic centre and Z = -0.89 kpc below the Galactic plane. We also calculated the mean cluster proper motion of (μα∗,μδ)=(-4.57 ± 0.29, -1.36 ± 0.27) mas yr-1. We derived an age of 3 Gyr and metallicity [Fe/H] = -0.5 ± 0.2 by the isochrone-fitting method, employing the PARSEC models. The total luminosity was derived in the Ks and V bands, finding MKs = -6.32 ± 1.10 mag and MV = -4.06 mag. Finally, the core and tidal radii were measured constructing the Garro 03 radial density profile and fitting the King model. We obtained rc = 3.07 ± 0.98 pc and rt = 19.36 ± 15.96 pc, respectively. Conclusions. We photometrically confirm the cluster nature for Garro 03, located in the Galactic disk. It is a distant, low-luminosity, metal-rich star cluster of intermediate age. We also searched for possible signatures (streams or bridges) between Garro 03 and Garro 01, but we exclude a companionship with the present analysis. We need spectroscopic data to classify it as an old open cluster or a young globular cluster, and to understand its origin.