The structure of the Milky Way based on unWISE 3.4 <i>μ</i>m integrated photometry

Mosenkov, Aleksandr V.; Савченко, С. С.; Smirnov, Anton A.; Camps, Peter

doi:10.1093/mnras/stab2445

Cited by 10 publications

(7 citation statements)

References 216 publications

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“…This behaviour is typical of a flared disc, as already detected in the Milky Way for both the stellar population and the gas (e.g. Grabelsky et al 1987;Feast et al 2014;López-Corredoira & Molgó 2014;Momany et al 2006;Reylé et al 2009;Li et al 2019;Mosenkov et al 2021). In the external regions, the disc population is detected up to 4 kpc from the plane (cf.…”

Section: Chemical Markers Of Milky Way Structuresupporting

confidence: 70%

GaiaData Release 3

Recio–Blanco¹,

Kordopatis²,

Laverny³

et al. 2023

A&A

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Context. The motion of stars has been used to reveal details of the complex history of the Milky Way, in constant interaction with its environment. Nevertheless, to reconstruct the Galactic history puzzle in its entirety, the chemo-physical characterisation of stars is essential. Previous Gaia data releases were supported by a smaller, heterogeneous, and spatially biased mixture of chemical data from ground-based observations. Aims. Gaia Data Release 3 opens a new era of all-sky spectral analysis of stellar populations thanks to the nearly 5.6 million stars observed by the Radial Velocity Spectrometer (RVS) and parametrised by the GSP-Spec module. In this work, we aim to demonstrate the scientific quality of Gaia's Milky Way chemical cartography through a chemo-dynamical analysis of disc and halo populations. Methods. Stellar atmospheric parameters and chemical abundances provided by Gaia DR3 spectroscopy are combined with DR3 radial velocities and EDR3 astrometry to analyse the relationships between chemistry and Milky Way structure, stellar kinematics, and orbital parameters.Results. The all-sky Gaia chemical cartography allows a powerful and precise chemo-dynamical view of the Milky Way with unprecedented spatial coverage and statistical robustness. First, it reveals the strong vertical symmetry of the Galaxy and the flared structure of the disc. Second, the observed kinematic disturbances of the disc -seen as phase space correlations-and kinematic or orbital substructures are associated with chemical patterns that favour stars with enhanced metallicities and lower [α/Fe] abundance ratios compared to the median values in the radial distributions. This is detected both for young objects that trace the spiral arms and older populations. Several α, iron-peak elements and at least one heavy element trace the thin and thick disc properties in the solar cylinder. Third, young disc stars show a recent chemical impoverishment in several elements. Fourth, the largest chemo-dynamical sample of open clusters analysed so far shows a steepening of the radial metallicity gradient with age, which is also observed in the young field population. Finally, the Gaia chemical data have the required coverage and precision to unveil galaxy accretion debris and heated disc stars on halo orbits through their [α/Fe] ratio, and to allow the study of the chemo-dynamical properties of globular clusters. Conclusions. Gaia DR3 chemo-dynamical diagnostics open new horizons before the era of ground-based wide-field spectroscopic surveys. They unveil a complex Milky Way that is the outcome of an eventful evolution, shaping it to the present day.

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Section: Chemical Markers Of Milky Way Structuresupporting

confidence: 70%

GaiaData Release 3

Recio–Blanco¹,

Kordopatis²,

Laverny³

et al. 2023

A&A

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“…Taking into account the uncertainty of distances may also solve the problem of establishing the form of the vertical distribution law f (ρ). Note that the analysis of the 2D distribution does not allow us to draw a definite conclusion about the functional form of this law (Mosenkov et al 2021).…”

Section: Resultsmentioning

confidence: 99%

“…One way to avoid this is to exclude the warp zone from consideration under the assumption that in the remaining area of the disk its average surface is flat: restrictions are imposed on the selection of tracers, for example, by the heliocentric distances r (e.g., r  4 kpc in Bobylev & Bajkova 2016a;r  4.5 kpc in Bobylev & Bajkova 2016b), by the predicted maximum warp offsets (<10 pc in Yao et al 2017) and by the distance R to the axis of rotation of the Galaxy (R < 7.0 kpc in Reid et al 2019). However, the exclusion of the warp zone requires the adoption of a specific warp model, and it is often taken as simple for this and other applications: the disk in the inner Galaxy (R R w ) is considered undisturbed, and in the outer one (R > R w ) it is usually represented by a combination of a power dependence on R and a simple trigonometric function of the azimuthal coordinate (e.g., Binney & Merrifield 1998;Pohl et al 2008;Xu et al 2015;Yao et al 2017;Romero-Gómez et al 2019;Cheng et al 2020;Mosenkov et al 2021). At the same time, to describe the warp in the outer Galaxy, in most of its morphological studies, simple symmetric models with a limited set of parameters are used-the radius R w at which the disk starts bending, the phase angle of the line-of-nodes and the maximum amplitude of the warp (see, e.g., Romero-Gómez et al 2019 and references therein).…”

Section: Introductionmentioning

confidence: 99%

“…That is why it seems important to us to abandon simplified warp models and consider the most general analytical warp model describing all the significant structural features of the middle surface of the disk identified by the tracers under consideration. The method of excluding the warp zone is also unsuccessful due to the presence of the disk flaring, which begins at R  R 0 , where R 0 is the Galactic center distance (e.g., Reid et al 2019;Mosenkov et al 2021), since the dependence of the dispersion parameter on the accepted boundaries of the area "undisturbed" by the warp appears.…”

Section: Introductionmentioning

confidence: 99%

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Modeling the Vertical Distribution of the Milky Way’s Flat Subsystem Objects

Nikiforov¹,

Usik²,

Veselova³

2023

Res. Astron. Astrophys.

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This paper is an initial stage of consideration of the general problem of joint modeling of the vertical structure of a Galactic flat subsystem and the average surface of the disk of the Galaxy, taking into account the natural and measurement dispersions. We approximate the average surface of the Galactic disk in the region covered by the data with a general (polynomial) model and determine its parameters by minimizing the squared deviations of objects along the normal to the model surface. The smoothness of the model, i.e. its order~$n$, is optimized. An outlier elimination algorithm is applied. The developed method allows us to simultaneously identify significant details of the Galactic warping and estimate the offset~$z_{\sun}$ of the Sun relative to the average (in general, non-flat) surface of the Galactic disk and the vertical scale of the object system under consideration for an arbitrary area of the disk covered by data. The method is applied to data on classical Cepheids (\citeauthor{Berdnikov+2000}, \citeauthor{Mel'nik+2015}). Significant local extremes of the average disk surface model were found based on Cepheid data: the minimum in the first Galactic quadrant and the maximum in the second. A well-known warp (lowering of the disk surface) in the third quadrant has been confirmed. The optimal order of the model describing all these warping details was found to be $n_\text{o}=4$. The local (for a small neighborhood of the Sun, $n_\text{o}=0$) estimate of $z_{\sun} = 28.1 \pm \left.6.1\right|_{\text{stat.}}\left.{}^{+1.3}_{-1.3}\right|_{\text{cal.}}$\,pc is close to the non-local (taking into account warping, $n_\text{o}=4$) $z_{\sun} = 27.1 \pm \left.8.8\right|_{\text{stat.}}\left.{}^{+1.3}_{-1.2}\right|_{\text{cal.}}$\,pc (statistical and calibration uncertainties are indicated), which suggests that the proposed modeling method eliminates the influence of warping on the $z_{\sun}$ estimate. However, the non-local estimate of the vertical standard deviation of Cepheids $\sigma_{\rho} = 132.0 \pm \left.3.7\right|_{\text{stat.}}\left.{}^{+6.3}_{-5.9}\right|_{\text{cal.}}$\,pc differs significantly from the local $\sigma_{\rho} = \left.76.5 \pm 4.4\right|_{\text{stat.}}\left.{}^{+3.6}_{-3.4}\right|_{\text{cal.}}$\, pc, which means the need to introduce more complex models for the vertical distribution outside the Sun's vicinity.

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“…As to the vertical distribution of dust in galaxies, an exponential law is also commonly used (see e.g., Verstappen et al 2013), but observational evidence for employing this law instead of, for example, a sech 2 -law is missing, mainly due to the poor resolution of contemporary FIR observations. Moreover, there is not even a consensus on which law to use for describing the stellar vertical distribution in galaxies (see Comerón et al 2011b, a review by van der Kruit & Freeman 2011, and a recent study on the Milky Way by Mosenkov et al 2021).…”

mentioning

confidence: 99%

The distribution of dust in edge-on galaxies: I. The global structure

Mosenkov¹,

Usachev²,

Shakespear³

et al. 2022

Preprint

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In this first paper in a series we present a study of the global dust emission distribution in nearby edge-on spiral galaxies. Our sample consists of 16 angularly large and 13 less spatially resolved galaxies selected from the DustPedia sample. To explore the dust emission distribution, we exploit the Herschel photometry in the range 100-500 𝜇m. We employ Sérsic and three-dimensional disc models to fit the observed two-dimensional profiles of the galaxies. Both approaches give similar results. Our analysis unequivocally states the case for the presence of extraplanar dust in between 6 to 10 large galaxies. The results reveal that both the disc scale length and height increase as a function of wavelength between 100 and 500 𝜇m. The dust disc scale height positively correlates with the dust disc scale length, similar to what is observed for the stellar discs. We also find correlations between the scale lengths and scale heights in the near-and far-infrared which suggest that the stellar discs and their dust counterparts are tightly connected. Furthermore, the intrinsic flattening of the dust disc is inversely proportional to the maximum rotation velocity and the dust mass of the galaxy: more massive spiral galaxies host, on average, relatively thinner dust discs. Also, there is a tendency for the dust-to-stellar scale height ratio to decrease with the dust mass and rotation velocity. We conclude that low-mass spiral galaxies host a diffuse, puffed-up dust disc with a thickness similar to that of the stellar disc.

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The structure of the Milky Way based on unWISE 3.4 μm integrated photometry

Cited by 10 publications

References 216 publications

GaiaData Release 3

GaiaData Release 3

Modeling the Vertical Distribution of the Milky Way’s Flat Subsystem Objects

The distribution of dust in edge-on galaxies: I. The global structure

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