220 research outputs found
Density biases and temperature relations for DESIRED HII regions
We present a first study based on the analysis of the DEep Spectra of Ionized
REgions Database (DESIRED). This is a compilation of 190 high signal-to-noise
ratio optical spectra of HII regions and other photoionized nebulae, mostly
observed with 8-10m telescopes and containing 29380 emission lines. We
find that the electron density ---- of the objects is underestimated
when [SII] and/or [OII] are
the only density indicators available. This is produced by the non-linear
density dependence of the indicators in the presence of density
inhomogeneities. The average underestimate is cm in
extragalactic HII regions, introducing systematic overestimates of ([OII]) and ([SII]) compared to ([NII]). The
high-sensitivity of [OII]
and [SII] to density makes them
more suitable for the diagnosis of the presence of high-density clumps. If
([NII]) is adopted, the density underestimate has a small impact in
the ionic abundances derived from optical spectra, being limited to up to
0.1 dex when auroral [SII] and/or [OII] lines are used. However, these
density effects are critical for the analysis of infrared fine structure lines,
such as those observed by the JWST in local star forming regions, implying
strong underestimates of the ionic abundances. We present temperature relations
between ([OIII]), ([ArIII]), ([SIII]) and
([NII]) for the extragalactic HII regions. We confirm a non-linear
dependence between ([OIII])-([NII]) due to a more rapid
increase of ([OIII]) at lower metallicities.Comment: Accepted for publication in MNRA
Hierarchical Star Formation: Stars and Stellar Clusters in the Gould Belt
We perform a study of the spatial and kinematical distribution of young open
clusters in the solar neighborhood, discerning between bound clusters and
transient stellar condensations within our sample. Then, we discriminate
between Gould Belt (GB) and local Galactic disk (LGD) members, using a previous
estimate of the structural parameters of both systems obtained from a sample of
O-B6 Hipparcos stars. Using this classified sample we analyze the spatial
structure and the kinematic behavior of the cluster system in the GB. The two
star formation regions that dominate and give the GB its characteristic
inclined shape show a striking difference in their content of star clusters:
while Ori OB1 is richly populated by open clusters, not a single one can be
found within the boundaries of Sco OB2. This is mirrored in the velocity space,
translating again into an abundance of clusters in the region of the kinematic
space populated by the members of Ori OB1, and a marginal number of them
associated to Sco OB2. In the light of these results we study the nature of the
GB with respect to the optical segment of the Orion Arm, and we propose that
the different content of star clusters, the different heights over the Galactic
plane and the different residual velocities of Ori OB1 and Sco OB2 can be
explained in terms of their relative position to the density maximum of the
Local Arm in the solar neighborhood. Although morphologically intriguing, the
GB appears to be the result of our local and biased view of a larger star
cluster complex in the Local Arm, that could be explained by the internal
dynamics of the Galactic disk.Comment: 23 pages, including 12 figures. Accepted for publication in MNRA
Bar pattern speeds in CALIFA galaxies: I. Fast bars across the Hubble sequence
The bar pattern speed () is defined as the rotational
frequency of the bar, and it determines the bar dynamics. Several methods have
been proposed for measuring . The non-parametric method
proposed by Tremaine \& Weinberg (1984; TW) and based on stellar kinematics is
the most accurate. This method has been applied so far to 17 galaxies, most of
them SB0 and SBa types. We have applied the TW method to a new sample of 15
strong and bright barred galaxies, spanning a wide range of morphological types
from SB0 to SBbc. Combining our analysis with previous studies, we investigate
32 barred galaxies with their pattern speed measured by the TW method. The
resulting total sample of barred galaxies allows us to study the dependence of
on galaxy properties, such as the Hubble type. We measured
using the TW method on the stellar velocity maps provided by
the integral-field spectroscopy data from the CALIFA survey. Integral-field
data solve the problems that long-slit data present when applying the TW
method, resulting in the determination of more accurate . In
addition, we have also derived the ratio of the corotation radius to
the bar length of the galaxies. According to this parameter, bars can be
classified as fast ( \cal{R}\%\cal{R}$ and the galaxy morphological
type. Our results indicate that independent of the Hubble type, bars have been
formed and then evolve as fast rotators. This observational result will
constrain the scenarios of formation and evolution of bars proposed by
numerical simulations.Comment: 17 pages, 10 figures, accepted for publication in A&
Functional upgrading in Chinaâs export processing sector
Functional upgrading occurs when a firm acquires more sophisticated functions within an existing value chain. In this paper, we analyze if there is evidence of this type of upgrading in Chinaâs export processing regime by investigating dynamics in the relative prevalence of Import & Assembly (IA) versus Pure Assembly (PA) processing trade over the period 2000-2013. Firms in both regimes provide similar manufacturing services to foreign companies, but IA firms also conduct the sophisticated tasks of quality control, searching, financing and storing imported materials. Consistent with a trend of functional upgrading, we show that the share of IA trade in total processing trade has increased rapidly during the period 2000-2006, both overall and within product categories. Furthermore, we find that this trend has gone hand in hand with improvements in a sectorâs labor productivity and unit values. Against expectations, we find that this process has slowed down notably during the period 2006-2013.status: publishe
Quantifying the energetics of molecular superbubbles in PHANGS galaxies
Star formation and stellar feedback are interlinked processes that
redistribute energy and matter throughout galaxies. When young, massive stars
form in spatially clustered environments, they create pockets of expanding gas
termed superbubbles. As these processes play a critical role in shaping galaxy
discs and regulating the baryon cycle, measuring the properties of superbubbles
provides important input for galaxy evolution models. With wide coverage and
high angular resolution (50-150 pc) of the PHANGS-ALMA CO (2-1) survey,
we can now resolve and identify a statistically representative number of
superbubbles with molecular gas in nearby galaxies. We identify superbubbles by
requiring spatial correspondence between shells in CO with stellar populations
identified in PHANGS-HST, and combine the properties of the stellar populations
with CO to constrain feedback models and quantify their energetics. We visually
identify 325 cavities across 18 PHANGS-ALMA galaxies, 88 of which have clear
superbubble signatures (unbroken shells, central clusters, kinematic signatures
of expansion). We measure their radii and expansion velocities using CO to
dynamically derive their ages and the mechanical power driving the bubbles,
which we use to compute the expected properties of the parent stellar
populations driving the bubbles. We find consistency between the predicted and
derived stellar ages and masses of the stellar populations if we use a
supernova blast wave model that injects energy with a coupling efficiency of
10%, whereas continuous models fail to explain stellar ages we measure. Not
only does this confirm molecular gas accurately traces superbubble properties,
but it also provides key observational constraints for superbubble models. We
also find evidence that the bubbles sweep up gas as they expand and speculate
that these sites have the potential to host new generations of stars.Comment: 21 pages, 15 figures, 3 tables. Accepted to A&A. Abstract abridged
for arXi
Shape of the oxygen abundance profiles in CALIFA face-on spiral galaxies
Y.A. acknowledges financial support from the RamĂłn y Cajal programme (RyC-2011-09461). Y.A. and A.I.D. acknowledge support from the project AYA2013-47742-C4-3-P from the Spanish MINECO, as well as the âStudy of Emission-Line Galaxies with Integral-Field Spectroscopyâ (SELGIFS) programme, funded by the EU (FP7-PEOPLE-2013-IRSES-612701). Support for L.G. is provided by the Ministry of Economy, Development, and Tourismâs Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. LG acknowledges support by CONICYT through FONDECYT grant 3140566. R.M.G.D. acknowledges support from the Spanish grant AYA2014-57490-P, and from the âJunta de AndalucĂaâ P12-FQM2828 project. RAM thanks the Spanish program of International Campus of Excellence Moncloa (CEI). IM and A.d.O. acknowledge support from the Spanish MINECO grant AYA2013-42227P. JMA acknowledges support from the European Research Council Starting Grant (SEDmorph, P.I. V. Wild). Support for MM has been provided by DGICYT grant AYA2013-47742-C4-4-P. PSB acknowledges support from the RamĂłn y Cajal programme, grant ATA2010-21322-C03-02 from the Spanish MINECO. CJW acknowledges support through the Marie Curie Career Grant Integration 303912.We measured the gas abundance profiles in a sample of 122 face-on spiral galaxies observed by the CALIFA survey and included all spaxels whose line emission was consistent with star formation. This type of analysis allowed us to improve the statistics with respect to previous studies, and to properly estimate the oxygen distribution across the entire disc to a distance of up to 3-4 disc effective radii (re). We confirm the results obtained from classical H ii region analysis. In addition to the general negative gradient, an outer flattening can be observed in the oxygen abundance radial profile. An inner drop is also found in some cases. There is a common abundance gradient between 0.5 and 2.0 re of αO/H =-0.075 dex/re with a scatter of Ï = 0.016 dex/re when normalising the distances to the disc effective radius. By performing a set of Kolmogorov-Smirnov tests, we determined that this slope is independent of other galaxy properties, such as morphology, absolute magnitude, and the presence or absence of bars. In particular, barred galaxies do not seem to display shallower gradients, as predicted by numerical simulations. Interestingly, we find that most of thegalaxies in the sample with reliable oxygen abundance values beyond ~2 effective radii (57 galaxies) present a flattening of the abundance gradient in these outer regions. This flattening is not associated with any morphological feature, which suggests that it is a common property of disc galaxies. Finally, we detect a drop or truncation of the abundance in the inner regions of 27 galaxies in the sample; this is only visible for the most massive galaxies.Publisher PDFPeer reviewe
Shape of the oxygen abundance profiles in CALIFA face-on spiral galaxies
Astronomy & Astrophysics 587 (2016): A70 reproduced with permission from Astronomy & AstrophysicsWe measured the gas abundance profiles in a sample of 122 face-on spiral galaxies observed by the CALIFA survey and included all spaxels whose line emission was consistent with star formation. This type of analysis allowed us to improve the statistics with respect to previous studies, and to properly estimate the oxygen distribution across the entire disc to a distance of up to 3-4 disc effective radii (re). We confirm the results obtained from classical H ii region analysis. In addition to the general negative gradient, an outer flattening can be observed in the oxygen abundance radial profile. An inner drop is also found in some cases. There is a common abundance gradient between 0.5 and 2.0 re of αO/H =-0.075 dex/re with a scatter of Ï = 0.016 dex/re when normalising the distances to the disc effective radius. By performing a set of Kolmogorov-Smirnov tests, we determined that this slope is independent of other galaxy properties, such as morphology, absolute magnitude, and the presence or absence of bars. In particular, barred galaxies do not seem to display shallower gradients, as predicted by numerical simulations. Interestingly, we find that most of thegalaxies in the sample with reliable oxygen abundance values beyond ~2 effective radii (57 galaxies) present a flattening of the abundance gradient in these outer regions. This flattening is not associated with any morphological feature, which suggests that it is a common property of disc galaxies. Finally, we detect a drop or truncation of the abundance in the inner regions of 27 galaxies in the sample; this is only visible for the most massive galaxiesWe acknowledge financial support from the Spanish Ministerio de EconomĂa y Competitividad (MINECO) via grant AYA2012-31935, and from the âJunta de AndalucĂaâ local government through the FQM-108 project. We also acknowledge support to the ConaCyt funding program 180125. Y.A. acknowledges fi- nantial support from the RamĂłn y Cajal programme (RyC-2011-09461). Y.A. and A.I.D. acknowledge support from the project AYA2013-47742-C4-3-P from the Spanish MINECO, as well as the âStudy of Emission-Line Galaxies with Integral-Field Spectroscopyâ (SELGIFS) programme, funded by the EU (FP7- PEOPLE-2013-IRSES-612701). Support for L.G. is provided by the Ministry of Economy, Development, and Tourismâs Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. LG acknowledges support by CONICYT through FONDECYT grant 3140566. R.M.G.D. acknowledges support from the Spanish grant AYA2014-57490-P, and from the âJunta de AndalucĂaâ P12-FQM2828 project. RAM thanks the Spanish program of International Campus of Excellence Moncloa (CEI). IM and A.d.O. acknowledge support from the Spanish MINECO grant AYA2013-42227P. JMA acknowledges support from the European Research Council Starting Grant (SEDmorph, P.I. V. Wild). Support for MM has been provided by DGICYT grant AYA2013-47742-C4-4-P. PSB acknowledges support from the RamĂłn y Cajal programme, grant ATA2010-21322-C03-02 from the Spanish MINECO. CJW acknowledges support through the Marie Curie Career Grant Integration 30391
- âŠ