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Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice Cedex 4, France Methods. We developed a method for systematically extracting the RC stars from a 2MASS ( J− K s, J) colour-magnitude diagram of 1°×1° bins in ℓ× b, covering the range 40°≤ ℓ≤320° and −10°≤ b≤10°. 2MASS data continue to be important because we are able to identify and trace the RC stars to much farther distances than in any optical survey of the Galactic disc. The foreground star contamination in the selected sample was removed using the accurate astrometric data from Gaia EDR3. We analysed the spiral arms and asymmetry in the Galaxy above and below the Galactic plane in galactocentric coordinates. from renumics import spotlight spotlight. show( df, dtype ={ "image": spotlight. Image, "embedding": spotlight. Embedding}) 🚀 Start with a use case Here, m J and m K s represent the apparent magnitude in J and K s bands. We assumed a Dirac delta luminosity function for K giant stars with an absolute magnitude M J and M K s of −0.945±0.01 and −1.606±0.009 ( Ruiz-Dern et al. 2018). The effect of metallicity on the absolute magnitude and intrinsic colours of RC stars observed in the SDSS Apache Point Observatory Galactic Evolution Experiment (APOGEE) and the GALactic Archaeology with HERMES (GALAH) was calculated in Plevne et al. (2020) by using the Bayesian-based distance from Bailer-Jones et al. (2018). The median colours of RC stars in the NIR bands J− K s=0.62±0.05 mag are the same for low- and high-metallicity RC stars. However, the median value of absolute magnitude in the J band shows a slight difference, M J=−1.05±0.21 for low- α RC stars, and M J=0.89±0.27 mag for high- α sources. The distance derived using these values of absolute magnitude and colours for the low and high metallicity in APOGEE RC sample ( Bovy et al. 2014) shows an offset of only ∼200 pc. Hence, it is safe to assume solar neighbourhood values of absolute magnitude and intrinsic colour in the NIR bands to calculate the distance. 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

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 asymmetry above and below the Galactic plane with respect to longitude has also been observed earlier in a few regions of the Galactic plane using various stellar tracers (e.g., López-Corredoira et al. 2002; Ferguson et al. 2017). We studied the continuous asymmetry, which is a manifestation of the warped disc of the Galaxy, with respect to longitude from 40°≤ ℓ≤320°. 5.3. Asymmetry in the spiral arms The Fitness Center (with floor-ceiling windows; has free weights, treadmills, elliptical machines; offers complimentary exercise classes); Courtyard Over-density map of RC stars above ( Z>0) and below ( Z<0) the Galactic plane, in panels a and b, respectively. The bottom panels represent the distribution of the ratio of RC stars above and below the Galactic plane in the galactocentric coordinate system with ℓ range of 40°≤ ℓ≤320° and −10°≤ b≤10° in panel c and | b| = 5° in panel d. The spiral-arm pattern (dot-dashed) follows the same colour codes as in Fig. 5. The vessel (IMO number 9008598) is currently Bahamas- flagged (MMSI 311085000) and registered in Nassau. History - construction and ownership Gaia Collaboration (Drimmel, R. et al.) 2023, A&A, in press, https://doi.org/10.1051/0004-6361/202243797 [GoogleScholar]

Overall, the errors on the distance determination include the errors in the absolute magnitude (0.5% contribution), extinction, and intrinsic colour (3% contribution) and the errors caused by assuming a Dirac delta luminosity function (5%). The photometric error has a negligible contribution for a mean magnitude in a bin with more than 50 stars. Including all the uncertainties, the error on the distance determination is smaller than 10%. A comparison of the distance estimated by our method with those provided by Gaia and APOGEE is made in Sect. 4.2. Using this method, we selected ∼10.5 million RC star candidates in the 40°≤ ℓ≤320° and −10°≤ b≤10° region. 3.2. ContaminationIt includes all the bug fixes and enhancements that were given to the executable and sprites.q3 within the last 4 years.

Gaia DR3 provides the astrophysical parameters, GSP-Phot (effective temperature, surface gravity, metallicity, absolute M G magnitude, radius, distance, and extinction) for a homogeneous sample of 471 million sources with G<19 mag ( Andrae et al. 2023). This is part of the results from the astrophysical parameter inference system (Apsis) within the Gaia Data Processing and Analysis Consortium. The parameters were calculated by simultaneously fitting BP/RP spectra, parallax, and G mag using Bayesian forward modelling based on isochrone models. One of the caveats of this approach is that the effective temperature-extinction degeneracy cannot be broken for red stars, as shown in Fig. 6a of Andrae et al. (2023). However, high-quality parallax data, that is, are expected to give reliable T eff and logg estimates for red giants or RC stars. Using only high-quality parallax data corresponding to our RC sample stars, we found a contamination of only ∼2% using log g>4 dex. The largest accommodations are the 3-Bedroom Grand Owners Suites (1375 ft2 / 128 m2, with included outdoor terrace). We developed an automated procedure for selecting candidate RC stars from 2MASS colour-magnitude diagrams in the Galactic disc (40°≤ ℓ≤320°, and −10°≤ b≤10°) avoiding the regions closer to the bulge (| ℓ|<40°). A large sample of RC stars (∼10 million) was retrieved from the 2MASS data with distance uncertainties smaller than 10% and a contamination rate < 20%. The spatial density distribution of RC stars in the Galactic disc is dominated by an exponentially decreasing density. However, we found an over-density in the RC stars that coincides with the Outer arm and Perseus arm. The Outer arm is continuously traced for the first time in the second and third Galactic quadrants up to ( X, Y)∼(−10,−10.5) kpc using RC stars. Significant enhancement in the stellar counts is also observed in the Perseus arm. This implies that the RC stars, representing the older population, are good tracers for mapping the outer arms. This is also supported by previous observations ( Benjamin et al. 2005; Churchwell et al. 2009). The inner arms might be traced by the younger population alone. The difference in the spiral structure that is traced by the younger and older population might represent the age gradient across the spiral arm, which favours the density wave theory for the spiral arm formation ( Vallée 2022).

The local density Σ( X, Y) and mean density ⟨Σ( X, Y)⟩ at ( X, Y) were calculated using the bi-variate kernel density estimator using a bandwidth of 0.3 and 2 kpc, respectively. The over-density map shown in Fig. 5b reveals some discernible arm-like features. We used the log-periodic spiral arm model from Reid et al. (2019); Eq. ( 4) to map the spiral arms in the RC over-density plot, AmphorA Restaurant (ship's dining room, open-seating; offers 5-course gourmet dinner menu which is changed daily; along with onboard-made bread, in all ports of call the executive chef goes to the local markets to shop for fresh ingredients) Follows the complete list of Star Legend lounges, clubs and other entertainment venues for kids, teens and adults. The details are spread around this forum under topics associated with hex editing, the sfc launcher, q3_editor and other tools. Marrese, P. M., Marinoni, S., Fabrizio, M., & Altavilla, G. 2022, https://gea.esac.esa.int/archive/documentation/GDR3/index.html, id. 15