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Some of the Webb Cycle 1 studies for galaxies will look at early galaxy formation, galaxies with "low metallicity" (rich in hydrogen and helium) and galaxy clusters to assist with its long-term quest to understand galactic evolution. While NASA did not directly say how this imagery will assist Webb, of note is the newer telescope's efforts to understand how galaxies were formed and evolved, particularly in the early universe. Here, the data types are discovered automatically from the dataset and we use a pre-defined layout for model debugging. Custom layouts can be built programmatically or via the UI.

R G and θ G in Eq. ( 4) are the galactocentric radius and azimuth (defined as 0 towards the Sun and increasing in the direction of Galactic rotation) along the arm, respectively. R G,ref, θ G,ref, and ψ are the reference galactocentric radius, azimuth, and pitch angle for a given arm. Castro-Ginard et al. (2021) determined the parameters for four arms (Perseus, Local, Sagittarius, and Scutum) by fitting the above model on the distribution of Galactic open clusters in Gaia EDR3 data and high-mass star-forming regions in the Galaxy from Reid et al. (2014). These parameters were used to construct the corresponding arm segments. The parameters of arms that were not considered (Norma and Outer arms) in Castro-Ginard et al. (2021) were taken from Reid et al. (2019). The galactocentric coordinates for corresponding arms were then calculated using the following equations: Recently, Lucey et al. (2020) have used available photometric data from Gaia DR2, PansTARRS, 2MASS, and ALLWISE to select the RC stars. They provided a sample of 2.6 million RC stars (L20 hereafter). Their method involves predicting astroseismic (Δ P, Δ ν) and spectroscopic parameters ( T eff, log g) obtained from the SED using neural networks. They divided their RC sample into two categories: stars with a contamination rate of 20% and a completeness of 25% as tier1, and stars with a contamination rate of 33% and a completeness rate of 94% as tier2. A cross-match of their catalogue with our candidate stars results in 73% overlap in our survey region. In a sub-classification, we are able to recover 85% of the more reliable stars of tier1 and 71% of tier2 stars. To have a clear idea of completeness, a colour-magnitude diagram of the low-extinction field 2MASS ℓ=45° and b=5° is shown in the lower panel of Fig. 3. L20 RC stars of this region and RC candidates from our sample are over-plotted in the same figure with blue and red points, respectively. Similar to the APOGEE RC, the missing L20 RC stars are mostly present on the redder side of the RC locus. The figure shows that increasing our colour selection criteria to 2 σ or 3 σ will increase the contamination. 4.2. Comparison of the estimated distance It includes all the bug fixes and enhancements that were given to the executable and sprites.q3 within the last 4 years. Hammersley, P. L., Cohen, M., Garzón, F., Mahoney, T., & López-Corredoira, M. 1999, MNRAS, 308, 333 In this paper, we present a systematic study to map the red clump (RC) stars over the whole Galactic plane, except for the bulge region, to trace the spiral arms and the asymmetry arising from the warp. The paper is organised as follows. The data used in our study to extract the RC sample are presented in Sect. 2. Section 3 describes the automatic selection procedure to isolate RC stars and the removal of contamination from the selected sample. Sample completeness with respect to other catalogues available in the literature and their distance comparison with our estimated values are discussed in Sect. 4. The results obtained by studying the distribution of the final RC star sample are discussed in Sect. 5. We summarise our study with a discussion and conclusions in Sect. 6. 2. Data

Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice Cedex 4, France If you would like to contribute to Spotlight, the easiest way is to have a look at our Contribution Docs and the CONTRIBUTING.md. The Marina (retractable watersports platform for water skiing, windsurfing, snorkeling, kayaking; the ship provides water rafts, wakeboards, paddleboards and a water trampoline island; the steel cage forms a swimming pool in the sea) Windstar's "Star Plus" project increased the fleet's capacity by 24%. The project (completed in 2021 October) resulted in bigger capacity (254 to 320 passengers, 140 to 190 crew), increased GT tonnage/volume (9975 to 12995 tons), increased length (134 to 159 m), more staterooms (106 to 156), adding new venues and public spaces, machinery upgrades (new Wartsila marine diesel engines). The project was scheduled for the period October 2019 through November 2020, at Fincantieri's shipyards in Palermo (Sicily Island, Italy) and Trieste (Italy). We built 2MASS colour-magnitude diagrams ( J− K s, J) in a region of 1 deg 2 around the central ℓ and b with boundaries of and . The majority of the stars lie on the main sequence or in giant phase in the CMDs. The most common types of giants are K giants; therefore, the redder dense region of the CMD corresponds to RC stars. The RC stars are distributed in the vertical and horizontal directions of the CMD by the effect of distance and extinction along the line of sight. Hence, instead of a clump, they appear as a band in the CMDs. The stars lying on the bluer side of the RC stars are predominantly foreground dwarf stars, and the redder regions contain M giant or AGB-type evolved stars at higher extinction and larger distance.

The powerplants were upgraded from 4x Bergen diesel engines (model B33:45, combined power output 7,3 MW) to 4x Wartsila engines (model Wartsila 46F, combined output 5 MW) running on the cleaner ULSD (ultra-low sulfur diesel) fuel.APOGEE has another value-added catalogue named ‘StarHorse’. It is dedicated to finding the distance, extinction, and astrophysical parameters of the stars by combining the high-resolution spectroscopic data from APOGEE with broadband photometric data (Pan-STARRS, 2MASS, and ALLWISE) and parallax ( Gaia EDR3) using Bayesian statistics ( Santiago et al. 2016; Queiroz et al. 2020). The StarHorse DR17 catalogues list 562 424 (RC as well as non-RC) APOGEE sources with distance uncertainties of ∼5%. The region 39.5°< ℓ≤320° and −10°≤ b≤10° contains 111 438 StarHorse stars. A cross-match of these stars with our catalogue in a 1″ sky region results in 45 580 stars in common. The distance comparison of the cross-matched stars obtained from our method ( x-axis) with the StarHorse median distance is shown in the bottom left panel of Fig. 4. Most of the stars lie close to the 1:1 line, with some scattering of the outliers.