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APOGEE and Gaia distances can only be used to compare nearby distances (< 3–5 kpc). On the other hand, The L20 catalogue provides the distances of 2.4 million stars with ∼75 000 stars at distances > 10 kpc by correcting for the extinction in the W1 WISE band. A comparison of the L20 distances with ours (bottom right panel of Fig. 4) shows that the vast majority of the stars are on a one-to-one correlation. The distance to the fainter stars seems to be overestimated in the L20 catalogue, which may result from an uncertain extinction in the W1 band. 5. Results

We also used data from the Gaia space-based telescope. Gaia early data release 3 (EDR3), ( Gaia Collaboration 2021) includes data for the first 34 months of its operational phase. Gaia EDR3 contains information about 1.8 billion sources ranging from 3 to 21 G-band magnitude. This data release contains the full astrometric data ( Lindegren et al. 2021) of 1.4 billion sources. We make use of the distance information of Gaia EDR3 stars ( Bailer-Jones et al. 2021), and astrophysical parameters from Gaia data release 3 (DR3), ( Andrae et al. 2023) to remove contamination by foreground and evolved stars. 3. RC sample selectionThe RC stars are low-mass core-helium-burning stars with a narrow range of intrinsic luminosity and colour in this phase ( Girardi 2016) of their evolution. This property makes them reliable distance indicators. The luminosity function derived in Hammersley et al. (1999) shows that at the peak of the red clump stars (K giants), there are about ten times more sources than stars either 0.8 mag brighter or fainter. Because they are a good distance indicator and are numerous in the Galaxy, they can be used to probe the structure of the intermediate-to-old Galactic disc. RC stars were selected by analysing 2MASS colour-magnitude diagrams (CMDs) constructed from 40°≤ ℓ≤320°, avoiding the bulge region and −10°≤ b≤10° with 1deg 2 binning, thus covering 5600 deg 2 fields. 3.1. Extraction of candidate RC stars from 2MASS CMDs 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. 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. To change the game's resolution, open your "SFC.INI" file and edit the entries below to one of the values above. In addition to the spiral features, the asymmetry in the disc structure due to the warping of the disc is also observed in various tracers (e.g., Kerr 1957; Henderson 1979; Drimmel & Spergel 2001; Nakanishi & Sofue 2003; López-Corredoira et al. 2002; Yusifov 2004; Marshall et al. 2006; Levine et al. 2006; Poggio et al. 2018; Chen et al. 2019; Chrobáková et al. 2022). However, the asymmetries in the spiral arms due to disc warping have not been studied so far.

Assuming ( López-Corredoira et al. 2002; Indebetouw et al. 2005), we calculated the distance ( d) and extinction ( A J) of each extracted RC star from Eqs. ( 1) and ( 2), 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. 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 section, the obtained RC sample is cross-matched with other RC star catalogues available in the literature to verify the completeness and distance determination. 4.1. Sample completeness 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 distanceHammersley, P. L., Cohen, M., Garzón, F., Mahoney, T., & López-Corredoira, M. 1999, MNRAS, 308, 333 The Fitness Center (with floor-ceiling windows; has free weights, treadmills, elliptical machines; offers complimentary exercise classes); Courtyard

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 distance of our selected stars matches the two APOGEE catalogues well. However, the APOGEE spectroscopic sample has a brightness limit of H<13 mag, which corresponds to stars only in nearby regions ( d<3–5 kpc). Hence, the APOGEE sample can be used to confirm the reliability of our catalogue distance to about 5 kpc. 4.2.2. Gaia distances The largest accommodations are the 3-Bedroom Grand Owners Suites (1375 ft2 / 128 m2, with included outdoor terrace).The vessel (IMO number 9008598) is currently Bahamas- flagged (MMSI 311085000) and registered in Nassau. History - construction and ownership We calculated the distance of RC stars by assuming the constant luminosity function of K-type giants within a 10% uncertainty level (as discussed in Sect. 3.1). The distance information of giant stars can also be obtained from available astrometric, spectroscopic, and photometric data. In this section, the distances obtained by different methods are compared with the estimated distance for RC stars listed in our sample. 4.2.1. APOGEE RC and StarHorse distances Bailer-Jones, C. A. L., Rybizki, J., Fouesneau, M., Demleitner, M., & Andrae, R. 2021, AJ, 161, 147 Follows the complete list of Star Legend lounges, clubs and other entertainment venues for kids, teens and adults.