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Small-Scale Star Formation As Revealed by VVVX Galactic Cluster Candidates

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Small-Scale Star Formation As Revealed by VVVX Galactic Cluster Candidates MNRAS 499, 3522–3533 (2020) doi:10.1093/mnras/staa3045 Advance Access publication 2020 October 2 Small-scale star formation as revealed by VVVX galactic cluster candidates J. Borissova ,1,2‹ R. Kurtev,1,2‹ N. Amarinho,3 J. Alonso-Garc´ıa,2,4 S. Ram´ırez Alegr´ıa,4‹ S. Bernal,1,2 N. Medina,1,2 A.-N. Chene´ ,5 V. D. Ivanov, 6 P. W. Lucas 7 and D. Minniti8 1 Instituto de F´ısica y Astronom´ıa, Universidad de Valpara´ıso, Av. Gran Bretana˜ 1111, Playa Ancha, Casilla 5030, Chile Downloaded from https://academic.oup.com/mnras/article/499/3/3522/5917430 by Universidad Andres Bello user on 26 August 2021 2Millennium Institute of Astrophysics (MAS), 7500000 Santiago, Chile 3Laboratorio´ Nacional de Astrof´ısica (LNA), Rua dos Estados Unidos, 154-Jardim das Nac¸oes,˜ 37504-364 Itajuba,´ Brazil 4Centro de Astronom´ıa (CITEVA), Universidad de Antofagasta, Avenida Angamos 601, 1240000 Antofagasta, Chile 5NOIRLab international Gemini Observatory, Northern Operations Center, 670 A’ohoku Place, Hilo, HI 96720, USA 6European Southern Observatory, Karl Schwarzschildstr 2, D-85748 Garching bei Munchen,¨ Germany 7Centre for Astrophysics, University of Hertfordshire, College Lane, Hatffeld AL10 9AB, UK 8Departamento de F´ısica, Facultad de Ciencias Exactas, Universidad Andes´ Bello, Av. Fernandez Concha 700, Las Condes, 7550000 Santiago, Chile Accepted 2020 September 28. Received 2020 September 28; in original form 2020 June 9 ABSTRACT We report a search and analysis of obscured cluster candidates in the ‘VISTA Variables in the Via Lactea eXtended (VVVX)’ ESO Public Survey area encompassing the region between 229◦.4 < l < 295◦.2 and −4◦.3 < b < 4◦.4 of the southern Galactic disc. We discover and propose 88 new clusters. We improve the completeness of the embedded cluster population in this region, adding small size (linear diameters of 0.2–1.4 pc) and relatively far objects (heliocentric distance between 2 and 4 kpc) to existing catalogues. Nine candidates are proposed to be older open cluster candidates. Three of them (VVVX CL 204, CL 207, CL 208) have sufficient numbers of well-resolved stellar members to allow us to determine some basic cluster parameters. We confirm their nature as older, low-mass open clusters. Photometric analysis of 15 known clusters shows that they have ages above 20 Myr, and masses below 2000 M: in general, their proper motions follow the motion of the disc. We outline some groups of clusters, most probably formed within the same dust complex. Broadly, our candidates follow the network of filamentary structure in the remaining dust. Thus, in this part of the southern disc of the Galaxy, we have found recent star formation, producing small size and young clusters, in addition to the well-known, massive young clusters, including NGC 3603, Westerlund 2, and the Carina Nebula Complex. Key words: Galaxy: disc – open clusters and associations: general – infrared: stars – submillimetre: ISM. VVV survey data (e.g. Borissova et al. 2011, 2014, 2018; Solin, 1 INTRODUCTION Haikala & Ukkonen 2014;Barbaelal.´ 2015;Ivanovetal.2017, The investigation of open star clusters has been very useful for the and references therein) through a variety of techniques. The future exploration of the disc of our own Milky Way. They are excellent searches with Gaia DR3 and the LSST are also expected to yield laboratories not only for stellar evolution theory, but also to test the large numbers of open clusters (e.g. The LSST Science Book, LSST star formation history and the structure of the Galactic disc (e.g. de Science Collaboration 2009). Grijs & Lepine´ 2010). The characterization of these open cluster candidates is often This is an active area of research where good progress is being tricky, as they are located at low Galactic latitudes where not made. In the optical regime, the Gaia mission has enabled dis- only the stellar density is high, but also the interstellar extinction covery of hundreds of cluster candidates, reviewed known clusters and reddening are problematic. It is not surprising that different and distinguished asterisms among objects previously reported as approaches have been taken to measure the physical parameters for stellar clusters (e.g. Cantat-Gaudin et al. 2018, 2019;Granetal. these clusters, often using vastly different datasets. Fortunately, the 2019; Cantat-Gaudin & Anders 2020). The near-infrared data allow large datasets now available allow us to shift from the analysis of access to more embedded and younger objects, completing the view single objects to the study of large samples like the ones produced obtained through optical data. The early discoveries done with the now by Gaia and VVV, and also LSST in the future. In particular, 2 MASS survey (e.g. Bica et al. 2003; Dutra et al. 2003; Froebrich, we can now try to trace the star formation patterns at different scales Scholz & Raftery 2007) have been recently complemented with across the Galactic disc. The near-IR offers advantages over optical wavelengths for these kinds of studies because it is less sensitive to reddening and extinc- E-mail: [email protected] (JB); [email protected] (RK); tion. Using the near-IR we can see for example, young, obscured [email protected] (SRA) clusters farther away, deeper into the Galactic plane, and can also C 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society Small-scale star formation from VVVX clusters 3523 2 SURVEY DATA The VVVX survey was launched in 2016 as an extension of the com- pleted VVV survey in order to enhance its legacy value. The VVVX provides a spatial coverage from l = 230◦ to l = 20◦ (7h <α<19h). The data were obtained with the 4.1-meter ESO VISTA telescope (Visual and Infrared Survey Telescope for Astronomy; Emerson, McPherson & Sutherland 2006) located at Cerro Paranal, Chile, with the 16-detector VIRCAM (VISTA Infrared CAMera; Dalton et al. ∼ × 2 2006). It has a 1 1.5 deg field of view, works in the 0.9–2.5 μm Downloaded from https://academic.oup.com/mnras/article/499/3/3522/5917430 by Universidad Andres Bello user on 26 August 2021 wavelength range, and has a pixel scale of 0.34 arcsec px−1. The data are reduced with the VISTA Data Flow System (VDFS; Emerson et al. 2004; Irwin et al. 2004) at the Cambridge Astro- nomical Survey Unit1 (CASU). Processed images and photometric catalogues are available from the ESO Science Archive2 and from the VISTA Science Archive3 (Cross et al. 2012). A single VIRCAM image, called pawprint, contains large gaps; six pawprints taken in a spatial offset pattern must be combined to Figure 1. The VVVX Survey area, investigated in this work. The blue and fill them in, obtaining a contiguous image, called tile. Each point of yellow squares show the VVVX outer disc fields. The numbers in each tile the sky is imaged at least twice within a tile, except of the outermost are its identification number (top) and the number of available KS epochs, as edges that are imaged once. The VVVX pawprints and tiles are of 2019 May 2. aligned along l and b. The total effective exposure time of the tiles are: 8 s in KS (for a single epoch), 24 s in H and 60 in J band. In order to obtain the best results in such a crowded environment, measure more accurate distances, that are less affected by reddening we extract our own point spread function (PSF) photometry on the uncertainties. There is a disadvantage, however: the background different regions of interest. This procedure is described in detail contamination in the near-IR is generally much larger than in the by Alonso-Garc´ıa et al. (2018) and Borissova et al. (2011, 2014) optical, because at shorter wavelengths the same extinction helps to and enhances the depth of CASU aperture photometry, typically by reduce the numbers of distant stars that can be detected. Thus, the 1–2 mag, along with the completeness of our data. The magnitudes, optical colour magnitude diagrams of nearby clusters often appear calibrated in the VISTA system, were transformed to the 2 MASS cleaner than the more distant ones that we are finding in the near- standard system, and the saturated stars (usually with K ≤ 11.5 mag, IR. Therefore, both optical and near-IR studies are worthwhile and S depending on crowding) were replaced with 2 MASS photometry, complementary. following Alonso-Garc´ıa et al. (2018). In this work, we take advantage of the near-IR VVVX survey, searching for distant [1.0 < D (kpc) < 10.0] young clusters at very low Galactic latitudes (−5◦ < b < +5◦) and use them to trace 3 CLUSTER SEARCH AND CANDIDATE small-scale star formation across their fields. This is the fourth SELECTION paper in our effort to study the obscured cluster population in We searched cluster candidates by means of visual inspection, as in the MW (Borissova et al. 2011, 2014, 2018), using the ‘VISTA our previous works (Borissova et al. 2011, 2014, 2018). The observed Variables in the V´ıa Lactea’´ (VVV) and the new ‘VVV eXtended’ images were retrieved from the CASU data base. Initially the K tiles (VVVX) surveys that cover ∼1700 deg2 of the inner MW bulge S were visually inspected, creating a preliminary list of candidates. and southern disc in ZYJHK bands (Minniti et al. 2010; Saito S The main criterion was the presence of a local overdensity with et al. 2012). The VVV/VVVX images have a pixel size of 0.34 respect to the surrounding area and (or) visually connected with any arcsec, smaller than 2 MASS (Two Micron All Sky Survey; Skrut- surrounding nebulosity.
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