AbstractParental investments in children's cognitive and noncognitive outcomes are deeply important to policymakers. However, because parental investments are arguably endogenous, estimating their importance empirically poses a challenge. To address this challenge, this paper exploits a rich and novel dataset, the China Family Panel Studies, and proposes a culture‐specific instrumental variable based on the Chinese zodiac. By comparing the outcomes of children born just before and just after the cutoff for a "lucky" (or 'unlucky') zodiac sign, we find that parents' investments have significant effects on offspring's development of both cognitive and noncognitive skills.
MARTON, George Iuliu/0000-0003-2469-4900; Ziolkowska, Oliwia/0000-0002-0696-2839; Wyrzykowski, Lukasz/0000-0002-9658-6151; Gromadzki, Mariusz/0000-0002-1650-1518; Zielinski, Pawel/0000-0001-6434-9429; Kiss, Csaba/0000-0002-8722-6875 ; WOS: 000563107500001 ; We present optical-infrared photometric and spectroscopic observations of Gaia 18dvy, located in the Cygnus OB3 association at a distance of 1.88 kpc. Gaia 18dvy was noted by the Gaia alerts system when its light curve exhibited a greater than or similar to 4 mag rise in 2018-2019. the brightening was also observable at mid-infared wavelengths. the infrared colors of Gaia 18dvy became bluer as the outburst progressed. Its optical and near-infrared spectroscopic characteristics in the outburst phase are consistent with those of bona fide FU Orionis-type young eruptive stars. the progenitor of the outburst is probably a low-mass K-type star with an optical extinction of similar to 3 mag. A radiative transfer modeling of the circumstellar structure, based on the quiescent spectral energy distribution, indicates a disk with a mass of 4 x 10(-3)M. Our simple accretion disk modeling implies that the accretion rate had been exponentially increasing for more than 3 yr until mid-2019, when it reached a peak value of 6.9 x 10(-6)M yr(-1). in many respects, Gaia 18dvy is similar to the FU Ori-type object HBC 722. ; European Research Council (ERC) under the European UnionEuropean Research Council (ERC) [716155]; Hungarian Academy of SciencesHungarian Academy of Sciences [LP2018-7/2019, KEP-7/2018]; Hungarian National Research, Development and Innovation Office [GINOP 2.3.2-15-2016-00003, PD-128360]; Polish NCN DAINA [2017/27/L/ST9/03221]; European CommissionEuropean CommissionEuropean Commission Joint Research Centre [730890]; Polish MNiSWMinistry of Science and Higher Education, Poland [DIR/WK/2018/12]; Research Council of LithuaniaResearch Council of Lithuania (LMTLT) [S-LL-19-2]; Ministry of Education, Science and Technological Development of the Republic of Serbia [176011]; DFGGerman Research Foundation (DFG) [SPP 1992, WA 1047/11-1]; MINECO (Spanish Ministry of Economy) [RTI2018-095076-B-C21]; Polish NCN MAESTRO [2014/14/A/ST9/00121] ; We thank the anonymous referee, whose questions and comments significantly improved the paper. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program under grant agreement No. 716155 (SACCRED), Lendulet LP2018-7/2019 and KEP-7/2018 of the Hungarian Academy of Sciences, GINOP 2.3.2-15-2016-00003 and PD-128360 of the Hungarian National Research, Development and Innovation Office, Polish NCN DAINA grant 2017/27/L/ST9/03221, European Commission's Horizon 2020 OPTICON grant 730890, Polish MNiSW grant DIR/WK/2018/12, grant No.S-LL-19-2 of the Research Council of Lithuania, Project No.176011 "Dynamics and kinematics of celestial bodies and systems" of the Ministry of Education, Science and Technological Development of the Republic of Serbia, DFG priority program SPP 1992 "Exploring the Diversity of Extrasolar Planets" (WA 1047/11-1), the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). the Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and is operated by the Institute for Space Studies of Catalonia (IEEC). MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. We acknowledge ESA Gaia, DPAC, and the Photometric Science Alerts Team. We thank Christina Conner, Megan Davis, Alessandro Dellarovere, Hannah Gallamore, Mira Ghazali, Aaron Kruskie, Dylan Mankel, Jesse Leahy-McGregor, Brandon McIntyre, Barrett Ross, Courtney Wicklund, and Evan Zobel for observing Gaia 18dvy at the Michigan State University Observatory. Based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Based on observations obtained with telescopes of the University Observatory Jena, which is operated by the Astrophysical Institute of the Friedrich-Schiller-University.
Context. The Sagittarius (Sgr) stream is one of the best tools that we currently have to estimate the mass and shape of our Galaxy. However, assigning membership and obtaining the phase-space distribution of the stars that form the tails of the stream is quite challenging. Aims. Our goal is to produce a catalogue of the RR Lyrae stars of Sgr and obtain an empiric measurement of the trends along the stream in sky position, distance, and tangential velocity. Methods. We generated two initial samples from the Gaia DR2 RR Lyrae catalogue: one selecting only the stars within ±20° of the orbital plane of Sagittarius (Strip), and the other resulting from application of the Pole Count Map (nGC3) algorithm. We then used the model-independent, deterministic method developed in this work to remove most of the contamination by detecting and isolating the stream in distance and proper motions. Results. The output is two empiric catalogues: the Strip sample (higher-completeness, lower-purity) which contains 11 677 stars, and the nGC3 sample (higher-purity, lower-completeness) with 6608 stars. We characterise the changes along the stream in all the available dimensions, namely the five astrometric dimensions plus the metallicity, covering more than 2π rad in the sky, and obtain new estimates for the apocentres and the mean [Fe/H] of the RR Lyrae population. Also, we show the first map of the two components of the tangential velocity thanks to the combination of distances and proper motions. Finally, we detect the bifurcation in the leading arm and report no significant difference between the two branches in terms of metallicity, kinematics, or distance. Conclusions. We provide the largest sample of RR Lyrae candidates of Sgr, which can be used as input for a spectroscopic follow-up or as a reference for the new generation of models of the stream through the interpolators in distance and velocity that we constructed. ; Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This project has received funding from the University of Barcelona's official doctoral program for the development of a R+D+i project under the APIF grant and from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 745617. This work was supported by the MINECO (Spanish Ministry of Economy) through grants ESP2016-80079-C2-1-R (MINECO/FEDER, UE) and ESP2014-55996-C2-1-R (MINECO/FEDER, UE) and MDM-2014-0369 of ICCUB (Unidad de Excelencia "María de Maeztu"). This project has received support from the DGAPA/UNAM PAPIIT program grant IG100319. The work reported on in this publication has been fully or partially supported by COST Action CA18104: MW-Gaia. CM acknowledges support from the ICC University of Barcelona visiting academic grants and thanks the Gaia UB team for hosting her during part of this research.
NGC 6067 is a young open cluster hosting the largest population of evolved stars among known Milky Way clusters in the 50–150 Ma age range. It thus represents the best laboratory in our Galaxy to constrain the evolutionary tracks of 5–7 M⊙ stars. We have used high-resolution spectra of a large sample of bright cluster members (45), combined with archival photometry, to obtain accurate parameters for the cluster as well as stellar atmospheric parameters. We derive a distance of 1.78 ± 0.12 kpc, an age of 90 ± 20 Ma and a tidal radius of 14.8 +6.8−3.2 arcmin. We estimate an initial mass above 5700 M⊙, for a present-day evolved population of two Cepheids, two A supergiants and 12 red giants with masses ≈6 M⊙. We also determine chemical abundances of Li, O, Na, Mg, Si, Ca, Ti, Ni, Rb, Y and Ba for the red clump stars. We find a supersolar metallicity, [Fe/H] = +0.19 ± 0.05, and a homogeneous chemical composition, consistent with the Galactic metallicity gradient. The presence of a Li-rich red giant, star 276 with A(Li) = 2.41, is also detected. An overabundance of Ba is found, supporting the enhanced s-process. The ratio of yellow to red giants is much smaller than 1, in agreement with models with moderate overshooting, but the properties of the cluster Cepheids do not seem consistent with current Padova models for supersolar metallicity. ; This research is partially supported by the Spanish Government Ministerio de Economía y Competitividad under grants BES 2013-065384 and AYA2015-68012-C2-2-P (MINECO/FEDER). AM acknowledges support from the Ministerio de Educación, Cultura y Deporte through grant PRX15/00030.
Facilities: Liverpool:2 m, FTN, OO:0.65, MLO:1 m, BAT, OAO:0.5 m, Swift, Mayall. Software: IRAF (v2.16.1; Tody 1993), Starlink (v2015B; Disney & Wallace 1982), APHOT (Pravec et al. 1994), HEASOFT (v6.16), XIMAGE (v4.5.1), XSPEC (v12.8.2; Arnaud 1996), XSELECT (v2.4c), R (R Development Core Team 2011). ; The Andromeda Galaxy recurrent nova M31N 2008-12a had been observed in eruption 10 times, including yearly eruptions from 2008 to 2014. With a measured recurrence period of Prec = 351 ± 13 days (we believe the true value to be half of this) and a white dwarf very close to the Chandrasekhar limit, M31N 2008-12a has become the leading pre-explosion supernova type Ia progenitor candidate. Following multi-wavelength follow-up observations of the 2013 and 2014 eruptions, we initiated a campaign to ensure early detection of the predicted 2015 eruption, which triggered ambitious ground- and space-based follow-up programs. In this paper we present the 2015 detection, visible to near-infrared photometry and visible spectroscopy, and ultraviolet and X-ray observations from the Swift observatory. The LCOGT 2 m (Hawaii) discovered the 2015 eruption, estimated to have commenced at August 28.28 ± 0.12 UT. The 2013–2015 eruptions are remarkably similar at all wavelengths. New early spectroscopic observations reveal short-lived emission from material with velocities ∼13,000 km s^−1, possibly collimated outflows. Photometric and spectroscopic observations of the eruption provide strong evidence supporting a red giant donor. An apparently stochastic variability during the early supersoft X-ray phase was comparable in amplitude and duration to past eruptions, but the 2013 and 2015 eruptions show evidence of a brief flux dip during this phase. The multi-eruption Swift/XRT spectra show tentative evidence of high-ionization emission lines above a high-temperature continuum. Following Henze et al. (2015a), the updated recurrence period based on all known eruptions is Prec = 174 ± 10 days, and we expect the next eruption of M31N 2008-12a to occur around 2016 mid-September. ; A.F.V., and V.P.G. acknowledge support from RFBR Grant No. 16 February 00758. J.F., J.J., and G.S. acknowledge support from Spanish Ministry of Economy and Competitiveness (MINECO) grant AYA2014-59084-P, the E.U. FEDER funds, and AGAUR/Generalitat de Catalunya grant SGR0038/2014. S.F. acknowledges support from the Russian Scientific Foundation (grant N 14-50-00043) and the Russian Government Program of Competitive Growth of Kazan Federal University. M. Henze acknowledges the support of the Spanish MINECO under grant FDPI-2013-16933. M. Hernanz acknowledges MINECO support under grant ESP2014-56003-R.K.H. was supported by the project RVO:67985815. J.P.O. and K.L.P. acknowledge funding from the UK Space Agency. VARMR acknowledges financial support from the Radboud Excellence Initiative. S.C.W. acknowledges a visiting research fellowship at LJMU. This work has been supported in part by NSF grant AST-1009566 and NASA grant HST-Go-14125.012. ; Peer-reviewed ; Post-print
Context. The Perseus OB1 association, including the h and χ Persei double cluster, is an interesting laboratory for the investigation of massive star evolution as it hosts one of the most populous groupings of blue and red supergiants (Sgs) in the Galaxy at a moderate distance and extinction. Aims. We discuss whether the massive O-type, and blue and red Sg stars located in the Per OB1 region are members of the same population, and examine their binary and runaway status. Methods. We gathered a total of 405 high-resolution spectra for 88 suitable candidates around 4.5 deg from the center of the association, and compiled astrometric information from Gaia DR2 for all of them. This was used to investigate membership and identify runaway stars. By obtaining high-precision radial velocity (RV) estimates for all available spectra, we investigated the RV distribution of the global sample (as well as different subsamples) and identified spectroscopic binaries (SBs). Results. Most of the investigated stars belong to a physically linked population located at d = 2.5 ± 0.4 kpc. We identify 79 confirmed or likely members, and 5 member candidates. No important differences are detected in the distribution of parallaxes when stars in h and χ Persei or the full sample are considered. In contrast, most O-type stars seem to be part of a differentiated population in terms of kinematical properties. In particular, the percentage of runaways among them (45%) is considerable higher than for the more evolved targets (which is lower than ∼5% in all cases). A similar tendency is also found for the percentage of clearly detected SBs, which already decreases from 15% to 10% when the O star and B Sg samples are compared, respectively, and practically vanishes in the cooler Sgs. Concerning this latter result, our study illustrates the importance of taking the effect of the ubiquitous presence of intrinsic variability in the blue-to-red Sg domain into account to avoid the spurious identification of pulsating stars as SBs. Conclusions. All but 4 stars in our working sample (including 10 O giants/Sgs, 36 B Sgs, 9 B giants, 11 A/F Sgs, and 18 red Sgs) can be considered as part of the same (interrelated) population. However, any further attempt to describe the empirical properties of this sample of massive stars in an evolutionary context must take into account that an important fraction of the O stars is or likely has been part of a binary/multiple system. In addition, some of the other more evolved targets may have also been affected by binary evolution. In this line of argument, it is also interesting to note that the percentage of spectroscopic binaries within the evolved population of massive stars in Per OB1 is lower by a factor 4−5 than in the case of dedicated surveys of O-type stars in other environments that include a much younger population of massive stars. ; We acknowledge funding from the Spanish Government Ministerio de Ciencia e Innovación through grants PGC-2018-091 3741-B-C211/C22, SEV 2015-0548, and CEX2019-000920-S and from the Canarian Agency for Research, Innovation and Information Society (ACIISI), of the Canary Islands Government, and the European Regional Development Fund (ERDF), under grant with reference ProID2017010115.
Tesis ( Maestría en Ciencias, especialista en Desarrollo Rural).-Colegio de Postgraduados, 2009. ; La organización comunitaria del poblado La Unión Reforma Soyaltepec, ubicado en la Mixteca alta oaxaqueña, ha realizado durante los últimos 10 años un proyecto social para la reforestación en tierras degradadas, las cuales habían sido abandonadas para su uso con fines agrícolas. El objetivo de la investigación es identificar, describir y contribuir a explicar la génesis y desarrollo del proceso social de organización local para promover y realizar la reforestación, mediante una iniciativa de búsqueda de tierras abandonadas y su cesión a la comunidad para tal fin; siendo dicha acción conceptualizada como reapropiación territorial. La metodología utilizó un enfoque mixto cualitativo y cuantitativo, mediante el primero se describieron 10 organizaciones intracomunitarias, como coadyuvantes para las actividades de reforestación y vinculación con organizaciones civiles, instituciones educativas, gubernamentales y comunidades; por su parte el análisis cuantitativo permitió estimar los resultados productivos de las plantaciones forestales de Pinus oaxacana. Los resultados muestran el interés comunitario para continuar con su proyecto de reforestación y mejora ambiental, mediante un Comité de reforestación. La disponibilidad para la cesión de tierras con fines de reforestación, ha conllevado al fortalecimiento organizativo y búsqueda de arreglos que motiven la donación de tierras mediante un proceso de reapropiación territorial de 40.7 ha, donadas por 12 personas. El 64% de la superficie esta plantada con Pinus oaxacana, en tres sitios, donde predominan tepetate blanco y tepetate amarillo. La autoridad local y Comité de reforestación tienen bien definidas sus funciones y responsabilidades, sin embargo, favorecer sus capacidades de planificación fortalecerá las relaciones con las redes sociales externas.________Community organization in the town of La Union Reforma Soyaltepec, in the High Oaxaca Mixteca, has, in the last 10 years, carried out a social reforestation project in degraded lands, which have been abandoned after their use for agricultural purposes. The aim is to describe and contribute to the explanation of the genesis and development of the local organizational process to carry out a reforestation, through a search of abandoned lands and their being granted for the community. This action is conceptualized as land reappropriation. The methodology used a quali-quantitative approach. Through the qualitative process, 10 intra-community organizations were described, as coadjutant for reforestation and linking activities with public organizations, educational and government institutions, among others. The quantitative analysis allowed to estimate the productive results of the forest plantations of Pinus oaxacana. There is a certain interest to continue with the project of reforestation and environmental improvement, through a reforestation committee. The readiness to grant the lands has favored the organizational strengthening and the search for arrangements that will promote land donations through a process of land reappropriation of 40.7 ha, given by 12 people. 64% of the surface is planted with Pinus oaxacana, in three sites, where the predominant soils are white tepetate (volcanic soil) and yellow tepetate. The evaluated variables, of diameter and height, show a direct and positive relation with the age of the plantation, as do other variables having to do with management and quality of the site. The functions and responsibilities of the local authorities and Reforestation Committee are well defined, however, favoring their planning capabilities would strengthen their relationships with external social networks.
The recurrent nova V745 Scorpii underwent its third known outburst on 2014 February 6. Infrared monitoring of the eruption on an almost daily basis, starting from 1.3 days after discovery, shows the emergence of a powerful blast wave generated by the high velocity nova ejecta exceeding 4000 km s(-1) plowing into its surrounding environment. The temperature of the shocked gas is raised to a high value exceeding 10(8) K immediately after outburst commencement. The energetics of the outburst clearly surpass those of similar symbiotic systems like RS Oph and V407 Cyg which have giant secondaries. The shock does not show a free-expansion stage but rather shows a decelerative Sedov-Taylor phase from the beginning. Such strong shock fronts are known to be sites for. gamma-ray generation. V745 Sco is the latest nova, apart from five other known novae, to show. gamma-ray emission. It may be an important testbed to resolve the crucial question of whether or not all novae are generically. gamma-ray emitters by virtue of having a circumbinary reservoir of material that is shocked by the ejecta rather than. gamma-ray generation being restricted to only symbiotic systems with a shocked red giant (RG) wind. The lack of a free-expansion stage favors V745 Sco to have a density enhancement around the white dwarf (WD), above that contributed by a RG wind. Our analysis also suggests that the WD in V745 Sco is very massive and a potential progenitor for a future SN Ia explosion. ; Department of Space, Government of India ; NSF AST-1211196 ; Astronomy
We present the detection of day-timescale periodic variability in the r-band lightcurve of newly outbursting FU Orionis-type object HBC 722, taken from >42 nights of observation with the CQUEAN instrument on the McDonald Observatory 2.1 m telescope. The optical/near-IR lightcurve of HBC 722 shows a complex array of periodic variability, clustering around 5.8-day (0.044 mag amplitude) and 1.28-day (0.016 mag amplitude) periods, after removal of overall baseline variation. We attribute the unusual number of comparable strength signals to a phenomenon related to the temporary increase in accretion rate associated with FUors. We consider semi-random "flickering," magnetic braking/field compression and rotational asymmetries in the disk instability region as potential sources of variability. Assuming that the 5.8-day period is due to stellar rotation and the 1.28-day period is indicative of Keplerian rotation at the inner radius of the accretion disk (at 2 R-star), we derive a B-field strength of 2.2-2.7 kG, slightly larger than typical T Tauri stars. If instead the 5.8-day signal is from a disk asymmetry, the instability region has an outer radius of 5.4 R-star, consistent with models of FUor disks. Further exploration of the time domain in this complicated source and related objects will be key to understanding accretion processes. ; University Continuing Fellowship ; Creative Research Initiative program of the National Research Foundation of Korea (NRFK) 2010-0000712 ; Korean government (MEST) ; Basic Science Research Program through the National Research Foundation of Korea (NRF) ; Ministry of Education, Science and Technology 2012-0002330 ; W. J. McDonald Postdoctoral Fellowship ; Astronomy
Obscuration and confusion conspire to limit our knowledge of the inner Milky Way. Even at moderate distances, the identification of stellar systems becomes compounded by the extremely high density of background sources. Here we provide a very revealing example of these complications by unveiling a large, massive, young cluster in the Sagittarius arm that has escaped detection until now despite containing more than 30 stars brighter than G = 13. By combining Gaia DR2 astrometry, Gaia and 2MASS photometry and optical spectroscopy, we find that the new cluster, which we name Valparaiso 1, located at ∼2.3 kpc, is about 75 Ma old and includes a large complement of evolved stars, among which we highlight the 4 d classical Cepheid CM Sct and an M-type giant that probably represents the first detection of an AGB star in a Galactic young open cluster. Although strong differential reddening renders accurate parameter determination unfeasible with the current dataset, direct comparison to clusters of similar age suggests that Valparaiso 1 was born as one of the most massive clusters in the Solar Neighbourhood, with an initial mass close to 104 M⊙. ; This research is partially supported by the Spanish Government under grants AYA2015-68012-C2-2-P and PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE). HMT is also supported by FCT - Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019, UIDB/04434/2020; UIDP/04434/2020, PTDC/FIS-AST/28953/2017, and POCI-01-0145-FEDER-028953. ANC is supported by the international Gemini Observatory, a program of NSF's NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation, on behalf of the Gemini partnership of Argentina, Brazil, Canada, Chile, the Republic of Korea, and the United States of America. JB and RK are partially funded by ANID ˆa˘A ¸S Millennium Science Initiative Program ˆa˘A ¸S ICN12 009 awarded to the Millennium Institute of Astrophysics MAS.
