Machine learning and engineering teams use Spotlight to understand and communicate on complex unstructured data problems. Here are some examples on publicly available datasets along with code snippets (👨‍💻), interactive demos (🕹️) and blog articles (📝): Modality Gaia Collaboration (Drimmel, R. et al.) 2023, A&A, in press, https://doi.org/10.1051/0004-6361/202243797 [GoogleScholar]

Marrese, P. M., Marinoni, S., Fabrizio, M., & Altavilla, G. 2022, https://gea.esac.esa.int/archive/documentation/GDR3/index.html, id. 15 Yusifov, I. 2004, in The Magnetized Interstellar Medium, eds. B. Uyaniker, W. Reich, & R. Wielebinski, 165 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 Colour-magnitude ( J, J− K s) diagram of 1°×1° field centred around ℓ=251° and b=0° (upper panel) and ℓ=45° and b=5° (lower panel) in grey crosses. RC stars in the APOGEE value-added catalogue and L20 tier1 and tier2 RC stars are over-plotted as open blue circles in the respective panels. RC stars selected by our method are represented by red points.

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The Fitness Center (with floor-ceiling windows; has free weights, treadmills, elliptical machines; offers complimentary exercise classes); Courtyard The 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

Follows the complete list of Star Legend lounges, clubs and other entertainment venues for kids, teens and adults. Comparison of the distance obtained from different methods: our method with APOGEE (in the upper left panel), Gaia EDR3 ( r pgeo) with APOGEE RC (in the upper right panel), our catalogue with StarHorse (bottom left), and L20 catalogue (bottom right). The inset histograms in each panel represent the difference in respective distances. import datasets from renumics import spotlight ds = datasets. load_dataset( 'renumics/emodb-enriched', split = 'all') 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. Star Legend itinerary program is based on Mediterranean cruises with departures from ports mainly in France, Italy, Spain. In Northern Europe, the Windstar Legend ship cruises in the Baltic Sea on Norwegian Fjords itineraries and to Iceland leaving from Denmark and the UK.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, To change the game's resolution, open your "SFC.INI" file and edit the entries below to one of the values above. The Wellness Centre (WindSpa, Beauty Salon, Gym). WindSpa (operated by Steiner) has treatment rooms (for massages), Saunas, Steam Rooms. 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. Contamination Distribution of the ratio of RC stars above and below the Galactic plane as a function of longitude in 1° bins of ℓ.

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 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). 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. 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. 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.

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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. 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), Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License ( https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.