103 research outputs found
New transit observations for HAT-P-30 b, HAT-P-37 b, TrES-5 b, WASP-28 b, WASP-36 b, and WASP-39 b
We present new transit light curves for planets in six extrasolar planetary
systems. They were acquired with 0.4-2.2 m telescopes located in west Asia,
Europe, and South America. When combined with literature data, they allowed us
to redetermine system parameters in a homogeneous way. Our results for
individual systems are in agreement with values reported in previous studies.
We refined transit ephemerides and reduced uncertainties of orbital periods by
a factor between 2 and 7. No sign of any variations in transit times was
detected for the planets studied.Comment: Submitted to Acta Astronomic
Transverse-spin-dependent azimuthal asymmetries of pion and kaon pairs produced in muon-proton and muon-deuteron semi-inclusive deep inelastic scattering
New Transit Observations for HAT-P-30 b, HAT-P-37 b, TrES-5 b, WASP-28 b, WASP-36 b and WASP-39 b
We present new transit light curves for planets in six extrasolar planetary systems. They were acquired with 0.4–2.2 m telescopes located in west Asia, Europe, and South America. When combined with literature data, they allowed us to redetermine system parameters in a homogeneous way. Our results for individual systems are in agreement with values reported in previous studies. We refined transit ephemerides and reduced uncertainties of orbital periods by a factor between 2 and 7. No sign of any variations in transit times was detected for the planets studied.Fil: Maciejewski, G.. Nicolaus Copernicus University; PoloniaFil: Dimitrov, D.. Bulgarian Academy Of Sciences; BulgariaFil: Mancini, L.. Max Planck Institute for Astronomy; Alemania. Osservatorio Astrofisico Di Torino; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Southworth, J.. Keele University; Reino UnidoFil: Ciceri, S.. Max Planck Institute For Astronomy; AlemaniaFil: D'Ago, G.. Istituto Internazionale per gli Alti Studi ; ItaliaFil: Bruni, I.. Osservatorio Astrofisico di Bologna; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Raetz, St.. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania. European Space Agency; Países BajosFil: Nowak, G.. Instituto de Astrofísica de Canarias; España. Nicolaus Copernicus University; Polonia. Universidad de La Laguna; EspañaFil: Ohlert, J.. University of Applied Sciences; Alemania. Michael Adrian Observatorium; AlemaniaFil: Puchalski, D.. Nicolaus Copernicus University; PoloniaFil: Saral, G.. Istanbul University; Turquía. University Of Geneva (ug);Fil: Derman, E.. Ankara University; TurquíaFil: Petrucci, Romina Paola. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Jofré, E.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Seeliger, M.. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; AlemaniaFil: Henning, T.. Max Planck Institute for Astronomy; Alemani
Complex AGN feedback in the Teacup galaxy. A powerful ionised galactic outflow, jet-ISM interaction, and evidence for AGN-triggered star formation in a giant bubble
The ~0.1 type-2 QSO J1430+1339 (the 'Teacup') is a complex galaxy showing
a loop of ionised gas ~10 kpc in diameter, co-spatial radio bubbles, a compact
(~1 kpc) jet, and outflow activity. We used VLT/MUSE optical integral field
spectroscopic observations to characterise the properties and effects of the
galactic ionised outflow from kpc up to tens of kpc scales and compare them
with those of the radio jet. We detect a velocity dispersion enhancement (>300
km/s) elongated over several kpc perpendicular to the radio jet, the AGN
ionisation lobes, and the fast outflow, similar to what is found in other
galaxies hosting compact, low-power jets, indicating that the jet strongly
perturbs the host ISM. The mass outflow rate decreases with distance from the
nucleus, from around 100 /yr in the inner 1-2 kpc to <0.1 /yr
at 30 kpc. The ionised mass outflow rate is ~1-8 times higher than the
molecular one, in contrast with what is often quoted in AGN. The driver of the
multi-phase outflow is likely a combination of AGN radiation and the jet. The
outflow mass-loading factor (~5-10) and the molecular gas depletion time
(<10 yr) indicate that the outflow can significantly affect the star
formation and the gas reservoir in the galaxy. However, the fraction of the
ionised outflow that is able to escape the dark matter halo potential is likely
negligible. We detect blue-coloured continuum emission co-spatial with the
ionised gas loop. Here, stellar populations are younger (<100-150 Myr) than in
the rest of the galaxy (~0.5-1 Gyr). This constitutes possible evidence for
star formation triggered at the edge of the bubble due to the compressing
action of the jet and outflow ('positive feedback'), as predicted by theory.
All in all, the Teacup constitutes a rich system in which AGN feedback from
outflows and jets, in both its negative and positive flavours, co-exist.Comment: 26 pages, 16 figures; Astronomy & Astrophysics, in pres
INSPIRE: INvestigating stellar population in RElics: II. First data release (DR1)
[Context] The INvestigating Stellar Population In RElics (INSPIRE) is an ongoing project targeting 52 ultra-compact massive galaxies at 0.1 2) through a short and intense star formation burst, and then have evolved passively and undisturbed until the present day. Relics provide a unique opportunity to study the mechanisms of star formation at high-z. [Aims] INSPIRE is designed to spectroscopically confirm and fully characterise a large sample of relics, computing their number density in the redshift window 0.1 < z < 0.5 for the first time, thus providing a benchmark for cosmological galaxy formation simulations. In this paper, we present the INSPIRE Data Release (DR1), comprising 19 systems with observations completed in 2020. [Methods] We use the methods already presented in the INSPIRE Pilot, but revisiting the 1D spectral extraction. For the 19 systems studied here, we obtain an estimate of the stellar velocity dispersion, fitting the two XSH arms (UVB and VIS) separately at their original spectral resolution to two spectra extracted in different ways. We estimate [Mg/Fe] abundances via line-index strength and mass-weighted integrated stellar ages and metallicities with full spectral fitting on the combined (UVB+VIS) spectrum. [Results] For each system, different estimates of the velocity dispersion always agree within the errors. Spectroscopic ages are very old for 13/19 galaxies, in agreement with the photometric ones, and metallicities are almost always (18/19) super-solar, confirming the mass-metallicity relation. The [Mg/Fe] ratio is also larger than solar for the great majority of the galaxies, as expected. We find that ten objects formed more than 75% of their stellar mass (M∗) within 3 Gyr from the big bang and classify them as relics. Among these, we identify four galaxies that had already fully assembled their M∗ by that time and are therefore 'extreme relics' of the ancient Universe. Interestingly, relics, overall, have a larger [Mg/Fe] and a more metal-rich stellar population. They also have larger integrated velocity dispersion values compared to non-relics (both ultra-compact and normal-size) of similar stellar mass. [Conclusions ]The INSPIRE DR1 catalogue of ten known relics is the largest publicly available collection, augmenting the total number of confirmed relics by a factor of 3.3, and also enlarging the redshift window. The resulting lower limit for the number density of relics at 0.17 < z < 0.39 is ρ ∼ 9.1 × 10-8 Mpc-3.CS is supported by an ‘Hintze Fellow’ at the Oxford Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation. CS, CT, FLB, AG, and SZ acknowledge funding from the INAF PRIN-INAF 2020 program 1.05.01.85.11. AFM has received financial support through the Postdoctoral Junior Leader Fellowship Programme from ‘La Caixa’ Banking Foundation (LCF/BQ/LI18/11630007). GD acknowledges support from CONICYT project Basal AFB-170002. DS is a member of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne
INSPIRE: INvestigating Stellar Population in RElics: I. Survey presentation and pilot study
[Context] Massive elliptical galaxies are thought to form through a two-phase process. At early times (z > 2), an intense and fast starburst forms blue and disk-dominated galaxies. After quenching, the remaining structures become red, compact, and massive (i.e. red nuggets). Then, a time-extended second phase, which is dominated by mergers, causes structural evolution and size growth. Given the stochastic nature of mergers, a small fraction of red nuggets survive, without any interaction, massive and compact until today: these are relic galaxies. Since this fraction depends on the processes dominating the size growth, counting relics at low-z is a valuable way of disentangling between different galaxy evolution models. [Aims] In this paper, we introduce the INvestigating Stellar Population In RElics (INSPIRE) Project, which aims to spectroscopically confirm and fully characterise a large number of relics at 0:1z0:5. We focus here on the first results based on a pilot study targeting three systems, representative of the whole sample. [Methods] For these three candidates, we extracted 1D optical spectra over an aperture of r = 0:4000, which comprises 30% of the galaxies’ light, and we obtained the line-of-sight integrated stellar velocity and velocity dispersion. We also inferred the stellar [/Fe] abundance from line-index measurements and mass-weighted age and metallicity from full-spectral fitting with single stellar population models. [Results] Two galaxies have large integrated stellar velocity dispersion values (250 km s), confirming their massive nature. They are populated by stars with super-solar metallicity and [/Fe]. Both objects have formed 80% of their stellar mass within a short (0:5:0 Gyr) initial star formation episode occurred only 1 Gyr after the Big Bang. The third galaxy has a more extendedstar formation history and a lower velocity dispersion. Thus we confirm two out of three candidates as relics. [Conclusions] This paper is the first step towards assembling the final INSPIRE catalogue that will set stringent lower limits on the number density of relics at z0:5, thus constituting a benchmark for cosmological simulations, and their predictions on number densities, sizes, masses, and dynamical characteristics of these objects.CS is supported by a Hintze Fellowship at the Oxford Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation. C.S. is also very grateful to Ortwin Gerhard and his ?Dynamics Group? at the Max-Planck-Institut f?r Extraterrestrische Physik (MPE, Garching by Munich) for interesting and constructive discussions. C.T., A.G., L.H. and S.Z. acknowledge funding from the INAF PRIN-SKA 2017 programme 1.05.01.88.04. G.D. acknowledges support from CONICYT project Basal AFB-170002. AFM has received financial support through the Postdoctoral Junior Leader Fellowship Programme from La Caixa Banking Foundation (LCF/BQ/LI18/11630007). N.R.N. acknowledges financial support from the One hundred top talent programme of Sun Yat-sen University, Grant N. 71000-18841229. D.S. is a member of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne
INSPIRE: INvestigating Stellar Population In RElics -- I. Survey presentation and pilot program
Massive ETGs are thought to form through a two-phase process. At early times,
an intense and fast starburst forms blue and disk-dominated galaxies. After
quenching, the remaining structures become red, compact and massive, i.e., 'red
nuggets'. Then, a time-extended second phase which is dominated by mergers,
causes structural evolution and size growth. Given the stochastic nature of
mergers, a small fraction of red nuggets survives, without any interaction,
massive and compact until today: relic galaxies. Since this fraction depends on
the processes dominating the size growth, counting relics at low-z is a
valuable way to disentangle between different galaxy evolution models. In this
paper, we introduce the INvestigating Stellar Population In RElics (INSPIRE)
Project, that aims at spectroscopically confirming and fully characterizing a
large number of relics at 0.1<z<0.5. We focus here on the first results based
on a pilot program targeting three systems, representative of the whole sample.
For these, we extract 1D optical spectra over an aperture comprising ~30 % of
the galaxies light, and obtain line-of-sight integrated stellar velocity and
velocity dispersion. We also infer the stellar [/Fe] abundance from
line-index measurements and mass-weighted age and metallicity from
full-spectral fitting with single stellar population models. Two galaxies have
large integrated stellar velocity dispersion values, confirming their massive
nature. They are populated by stars with super-solar metallicity and
[/Fe]. Both objects have formed >80 % of their stellar mass within a
short (0.5 - 1.0 Gyrs) initial star formation episode occurred only ~1 Gyr
after the Big Bang. The third galaxy has a more extended star formation history
and a lower velocity dispersion. Thus we confirm two out of three candidates as
relics.Comment: 19 pages, 14 figures, accepted for publication in A&
INSPIRE: INvestigating Stellar Population In RElics II. First Data Release (DR1)
The INvestigating Stellar Population In RElics is an on-going project
targeting 52 ultra-compact massive galaxies at 0.1<z<0.5 with the X-Shooter@VLT
spectrograph (XSH). These objects are the perfect candidates to be 'relics',
massive red-nuggets formed at high-z (z>2) through a short and intense star
formation burst, that evolved passively and undisturbed until the present-day.
Relics provide a unique opportunity to study the mechanisms of star formation
at high-z. In this paper, we present the first INSPIRE Data Release, comprising
19 systems with observations completed in 2020. We use the methods already
presented in the INSPIRE Pilot, but revisiting the 1D spectral extraction. For
these 19 systems, we obtain an estimate of the stellar velocity dispersion,
fitting separately the two UVB and VIS XSH arms at their original resolution.
We estimate [Mg/Fe] abundances via line-index strength and mass-weighted
integrated stellar ages and metallicities with full spectral fitting on the
combined spectrum. Ages are generally old, in agreement with the photometric
ones, and metallicities are almost always super-solar, confirming the
mass-metallicity relation. The [Mg/Fe] ratio is also larger than solar for the
great majority of the galaxies, as expected. We find that 10 objects have
formed more than 75% of their stellar mass (M*) within 3 Gyr from the Big Bang
and classify them as relics. Among these, we identify 4 galaxies which had
already fully assembled their M* by that time. They are therefore `extreme
relics' of the ancient Universe. The INSPIRE DR1 catalogue of 10 known relics
to-date augment by a factor of 3.3 the total number of confirmed relics, also
enlarging the redshift window. It is therefore the largest publicly available
collection. Thanks to the larger number of systems, we can also better quantify
the existence of a 'degree of relicness', already hinted at the Pilot Paper.Comment: (Abstract abridged) 21 pages, 12 figures and 5 tables in the main
body, plus 3 figure and 1 table in the appendix, accepted for publication on
A&A. The associated data are available via the ESO Phase 3 Science Porta
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