adsabs/AstroCLIMB huggingface dataset:
Paper: DESI z ≳ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ∼ 4.7–6.6
Authors: Jinyi Yang, Xiaohui Fan, Ansh Gupta, Adam D. Myers, Nathalie Palanque-Delabrouille, Feige Wang, Christophe Yèche, Jessica Nicole Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Kyle Dawson, Axel de la Macorra, Arjun Dey, Govinda Dhungana, Kevin Fanning, Andreu Font-Ribera, Satya Gontcho, Julien Guy, Klaus Honscheid, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Laurent Le Guillou, Michael Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Edward Schlafly, Gregory Tarlé, Mariana Vargas Magana, Benjamin Alan Weaver, Risa Wechsler, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Top: the riz color–color diagram used for the quasar selection. The blue solid line shows the color track of quasars from z = 4.8 to z = 6.8 with a step of 0.1 (blue filled circles). The red points on the track represent quasars at z = 5.0, 5.5, 6.0, and 6.5. The blue crosses denote all existing quasars known at 4.8 ≤ z ≤ 6.8 (e.g., Fan et al. 2006; Willott et al. 2010; Mortlock et al. 2011; Venemans et al. 2015; Wu et al. 2015; Bañados et al. 2016, 2018; Jiang et al. 2016; Mazzucchelli et al. 2017; McGreer et al. 2018; Matsuoka et al. 2019a, 2019b; Pâris et al. 2017; Reed et al. 2019; Wang et al. 2016, 2018, 2019, 2021; Yang et al. 2017, 2019a, 2019b, 2020a, 2021), while the gray points and the black squares show the loci of M and L/T dwarfs (Kirkpatrick et al. 2011; Mace 2014; Best et al. 2015), respectively. The orange dashed lines bound the selected regions for z ∼ 5 and z ∼ 6 quasar candidates. Bottom: the zW1W2 color–color diagram. All symbols are the same as in the top panel. The orange dashed lines represent the cuts used for z ∼ 5 and z ∼ 6 quasar candidates. A more stringent z − W1 cut (orange dotted line) is used for the selection of z > 6.4 quasars. Note that the photometry in W1 and W2 are in the Vega system (W1Vega  =  W1AB − 2.699, W2Vega  =  W2AB − 3.339).
Paper: DESI z ≳ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ∼ 4.7–6.6
Authors: Jinyi Yang, Xiaohui Fan, Ansh Gupta, Adam D. Myers, Nathalie Palanque-Delabrouille, Feige Wang, Christophe Yèche, Jessica Nicole Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Kyle Dawson, Axel de la Macorra, Arjun Dey, Govinda Dhungana, Kevin Fanning, Andreu Font-Ribera, Satya Gontcho, Julien Guy, Klaus Honscheid, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Laurent Le Guillou, Michael Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Edward Schlafly, Gregory Tarlé, Mariana Vargas Magana, Benjamin Alan Weaver, Risa Wechsler, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption:                         Examples of the DESI spectra for quasars at z = 5, 6, and 6.5, binned with 7 pixels. The three spectra are from observations with ∼800–1000 s actual exposure time. These three quasars are 20.55, 20.72, and 21.20 mag in the Legacy Survey z band. The quasar broad emission lines (i.e., Lyβ, Lyα, O I, Si IV, and C IV) used for redshift measurements are marked with blue dotted lines. The spectra of all 412 new quasars are shown in Figure 7.
Paper: DESI z ≳ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ∼ 4.7–6.6
Authors: Jinyi Yang, Xiaohui Fan, Ansh Gupta, Adam D. Myers, Nathalie Palanque-Delabrouille, Feige Wang, Christophe Yèche, Jessica Nicole Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Kyle Dawson, Axel de la Macorra, Arjun Dey, Govinda Dhungana, Kevin Fanning, Andreu Font-Ribera, Satya Gontcho, Julien Guy, Klaus Honscheid, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Laurent Le Guillou, Michael Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Edward Schlafly, Gregory Tarlé, Mariana Vargas Magana, Benjamin Alan Weaver, Risa Wechsler, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: The z P1 y P1 W1 color–color diagram, used for the selection of z ∼ 6 and 6.5 quasars. All symbols are the same as Figure 1. A y P1 − W1 cut is applied for all objects, and the two regions separated by the z P1 − y P1 color (vertical orange dashed line) are the selections for z ∼ 6 and z > 6.4 quasar candidates, respectively.
Paper: DESI z ≳ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ∼ 4.7–6.6
Authors: Jinyi Yang, Xiaohui Fan, Ansh Gupta, Adam D. Myers, Nathalie Palanque-Delabrouille, Feige Wang, Christophe Yèche, Jessica Nicole Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Kyle Dawson, Axel de la Macorra, Arjun Dey, Govinda Dhungana, Kevin Fanning, Andreu Font-Ribera, Satya Gontcho, Julien Guy, Klaus Honscheid, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Laurent Le Guillou, Michael Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Edward Schlafly, Gregory Tarlé, Mariana Vargas Magana, Benjamin Alan Weaver, Risa Wechsler, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: A stacked histogram presenting the redshift distribution of new quasars (red, “New QSOs”) from this survey, compared with all existing known quasars that are in the DESI footprint and within our survey depth (i.e., < 21.5 in the LS z band). Known quasars that pass our selections are shown in orange (“Selected known QSOs”), while the quasars that do not meet our selections are in the color of blue (“Non-sel Known QSOs”). The redshift range that our survey focuses on has been marked in red (z = 4.8–6.8).
Paper: DESI z ≳ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ∼ 4.7–6.6
Authors: Jinyi Yang, Xiaohui Fan, Ansh Gupta, Adam D. Myers, Nathalie Palanque-Delabrouille, Feige Wang, Christophe Yèche, Jessica Nicole Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Kyle Dawson, Axel de la Macorra, Arjun Dey, Govinda Dhungana, Kevin Fanning, Andreu Font-Ribera, Satya Gontcho, Julien Guy, Klaus Honscheid, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Laurent Le Guillou, Michael Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Edward Schlafly, Gregory Tarlé, Mariana Vargas Magana, Benjamin Alan Weaver, Risa Wechsler, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: The spectra of new quasars from the SV1 selection ordered as in Table 2. The y-axis shows the flux density (f  λ ) in units of 10−17 erg s−1 cm−2 Å−1. The spectra have been binned with 11 pixels for the purpose of plotting. The blue vertical lines denote the observed wavelengths of the emission lines, including (from left to right) Lyβ, Lyα, O I, Si IV, and C IV. Quasar J0548–2233 is an example of WL quasar, and J0719+4249 is an example of BAL quasar.
Paper: DESI z ≳ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ∼ 4.7–6.6
Authors: Jinyi Yang, Xiaohui Fan, Ansh Gupta, Adam D. Myers, Nathalie Palanque-Delabrouille, Feige Wang, Christophe Yèche, Jessica Nicole Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Kyle Dawson, Axel de la Macorra, Arjun Dey, Govinda Dhungana, Kevin Fanning, Andreu Font-Ribera, Satya Gontcho, Julien Guy, Klaus Honscheid, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Laurent Le Guillou, Michael Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Edward Schlafly, Gregory Tarlé, Mariana Vargas Magana, Benjamin Alan Weaver, Risa Wechsler, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: The DESI spectrum of a z = 5.04 quasar J112903.54+023706.9, coadded from four exposures with a total exposure time of ∼4400 s. The spectrum plotted here is binned with 3 pixels for the BAL absorption measurements. The gray line is the spectral uncertainty. The target has a z-band magnitude of 21.3. This spectrum has sufficient S/N for quasar classification and study of strong absorption features. The Si IV and C IV BAL absorption troughs are denoted by the blue-shaded regions.
Paper: DESI z ≳ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ∼ 4.7–6.6
Authors: Jinyi Yang, Xiaohui Fan, Ansh Gupta, Adam D. Myers, Nathalie Palanque-Delabrouille, Feige Wang, Christophe Yèche, Jessica Nicole Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Kyle Dawson, Axel de la Macorra, Arjun Dey, Govinda Dhungana, Kevin Fanning, Andreu Font-Ribera, Satya Gontcho, Julien Guy, Klaus Honscheid, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Laurent Le Guillou, Michael Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Edward Schlafly, Gregory Tarlé, Mariana Vargas Magana, Benjamin Alan Weaver, Risa Wechsler, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: The DESI spectrum of a z = 5.03 quasar J100828.30−021229.8 without binning. The gray line represents the spectral uncertainty. A DLA system at z = 4.018 (red dashed line) is clearly present in the absorption spectrum. Its redshift is estimated using metal lines. The Voigt profile fitting (inset plot) yields a column density of ﹩\mathrm{log}\,{N}_{\mathrm{HI}}\,=\,21.2\pm 0.2﹩.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: The relationship between stellar mass and metallicity. The red points represent galaxies at z = 4–10, including the filled circles, pentagons, and diamonds, which respectively represent the ERO, GLASS, and CEERS objects analyzed in this paper. Red circles denote galaxies whose metallicities are determined using the direct T  e  method. The large red stars represent the average relationship for the ERO, GLASS, and CEERS objects in three equally separated mass ranges (M ⋆ = 107–108, 108–109, and 109–1010 M ⊙), along with the best-fit function shown as a thick long-dashed line (Equation (1)). Emerald green open pentagons show the average relation at z = 3–10 based on the JADES+CEERS sample (Curti et al. 2023b). Other red symbols represent high-redshift objects compiled from the literature, including open right-pointing triangles for NIRSpec DDT objects (Williams et al. 2023; Heintz et al. 2022; Langeroodi et al. 2022), left-pointing triangles for four NIRCam objects (Sun et al. 2022a, 2022b), an open hexagram for the stacked EIGER object (Matthee et al. 2023), and crosses for ALMA objects (Jones et al. 2020). Additionally, the relationship at lower redshift is displayed, including SDSS stacked galaxies in the local Universe shown as a gray dashed curve (Andrews & Martini 2013), and those at z ∼ 2.3 with gray open triangles and ∼3.3 with gray open squares (best fits shown as gray dotted–dashed curves; Sanders et al. 2021). The curves are displayed in the mass ranges explored in the original papers. These low-redshift metallicities are based on the direct T  e  method.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: The MZ relation in three different redshift bins: (a) z = 4–6, (b) z = 6–8, and (c) z = 8–10. The red symbols and the best-fit function (Equation (1)) are as shown in Figure 10. The large stars represent the average MZ relation rederived in each redshift bin, by splitting the sample into two groups based on stellar mass to have equal numbers of galaxies. For the JADES+CEERS relation (Curti et al. 2023b in emerald green), we plot their z = 3–6 subsample relation in panel (a), while adopt the z = 6–10 relation in panels (b) and (c). In addition, the cosmological simulation results at z = 5, 7, and 9 are displayed in panels (a), (b), and (c), respectively: FIRE in black (Ma et al. 2016), ILLUSTRISTNG in green (Torrey et al. 2019), FIRSTLIGHT in blue (Langan et al. 2020 in the low-mass regime with solid curves; and Nakazato et al. 2023 in the high-mass regime with shades), ASTRAEUS in yellow (Ucci et al. 2023), and FLARES in magenta (Wilkins et al. 2023). Some extrapolations are applied, as detailed in the text.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Left: (a) SFR dependence of the MZ (SFR–MZ) relation. The symbols and curves are consistent with those in Figure 10, including the average points, which are based on the three mass ranges that are equally separated. The coefficient of 0.66 for the combination of stellar mass and SFR is as indicated by Andrews & Martini (2013) in the local Universe, down to M ⋆ ∼ 107.4 M ⊙. Stacked galaxies at z = 2–3 with T  e -based metallicities are also suggested to fall on the z ∼ 0 relation in this parameter space (Sanders et al. 2021). Notably, the JWST objects analyzed in this study at z = 4–10 (red) also fall on the same SFR–MZ relation on average. A consistent view is obtained with the JADES+CEERS average points at z = 3–10 (emerald green; Curti et al. 2023b). Right: (b) metallicity difference from the SFR–MZ relation of Andrews & Martini (2013; ﹩{\rm{\Delta }}\mathrm{log}﹩ (O/H) = observed − predicted metallicity) for different redshift sources. The symbols are consistent with panel (a), except for the average points (large red stars), which are recalculated in this panel to represent the average ﹩{\rm{\Delta }}\mathrm{log}﹩ (O/H) values for the objects found in three different redshift bins, z = 4–6, 6–8, and 8–10. For the JADES+CEERS sample, average points of three mass bins are plotted for the two subsamples at z = 3–6 and 6–10, as found in Figure 11. This plot illustrates that no evolution is seen up to z ∼ 8, but a significant decrease in metallicity is observed beyond z > 8, albeit with a small sample size in this highest-redshift bin.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Comparison of the metallicity relationships with strong line ratios (R23, R3, R2, O32, and Ne3O2 from top left to bottom right) for ERO (circles), GLASS (pentagons), and CEERS (diamonds) galaxies with metallicity measurements based on the direct T  e  method. Each data point is color coded by its EW(Hβ) value, if available, as shown in the legend. The black dashed, long dashed, and dotted–dashed curves represent the metallicity relationships from Maiolino et al. (2008), Curti et al. (2017, 2020), and Bian et al. (2018), respectively. The blue and orange curves show the functions derived in Nakajima et al. (2022) for low-metallicity galaxies, with blue representing high-ionization galaxies (EW(Hβ) > 200 Å) and orange representing low-ionization galaxies (EW(Hβ) < 100 Å). Each curve is shown only within the metallicity range explored in the original paper.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Left: (a) similar to the left panel of Figure 13, but with the regions of μ 0.66 explored and unexplored by the original paper of Andrews & Martini (2013) highlighted. The blue solid curve represents the best-fit 2D projection of the SFR–MZ relation by Andrews & Martini (2013), determined down to μ 0.66 ∼ 7.5, with extrapolation toward lower mass shown by the dotted curve. Among the JWST objects, 83% have μ 0.66 > 7.5 and can be directly compared with the Andrews & Martini (2013) relation. Right: (b) similar to the left panel, but with a different coefficient of 0.55 adopted for the combination of mass and SFR on the abscissa axis, as presented by Curti et al. (2020). The blue solid curve represents the best-fit 2D projection of Curti et al. (2020)'s SFR–MZ relation, determined down to μ 0.55 ∼ 8.5, and extrapolated toward lower mass with the dotted curve. Only approximately 15% of the JWST objects have μ 0.55 > 8.5, and as such, the vast majority of the sample occupies a parameter space that is not explored by Curti et al. (2020).
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Comparison of literature determinations of electron temperature (T  e ) for four ERO galaxies (04590 in red, 06355 in orange, 10612 in green, and 05144 in emerald green) where [O III] λ4363 is identified. Different symbols indicate different publications, as shown in the legend. For the measurements of Arellano-Córdova et al. (2022), we show the average values based on the two spectra (i.e., two observing blocks: o007 and o008) for 06355 and 10612, but refer only to the o008 value for 04590. For each object, the symbols are slightly offset in the horizontal direction for display purposes. Some of the measurements in the literature do not present uncertainties and are plotted without error bars in the vertical direction.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: The relationship between stellar mass and SFR, with the SFRs derived based on the total Hβ luminosity (as described in the text) for use in the SFR–MZ relation. The symbols used are consistent with those in Figure 10. The background lines represent sSFR values ranging from 10−9 to 10−6 yr−1, from bottom to top. The JWST objects are distributed along the sequence of sSFR values around 10−8–10−7 yr−1.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Comparison between the MZ relation obtained in this study for ERO objects at z = 6.3–8.5 using T  e -based metallicities (colored circles) and those reported in the literature. Different symbol colors indicate different objects, as shown in Figure 6, and different symbols represent different publications, as indicated in the legend. For the metallicities from Arellano-Córdova et al. (2022), we show the average values based on the two spectra (i.e., two observing blocks: o007 and o008) for 06355 and 10612, but refer only to the o008 value for 04590. For the relationships of Schaerer et al. (2022) and Curti et al. (2023a), the stellar masses are adopted as originally estimated in each paper. For the others where stellar masses are referenced from other studies, we show the two stellar masses from Carnall et al. (2023) and Tacchella et al. (2023) for each object (only Carnall et al. 2023 for 05144). The comparison confirms the good agreement between our measurements and earlier results on the MZ relation.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Empirical metallicity indicator using both R23 and O32 as proposed by Izotov et al. (2019, 2021) in the low-metallicity regime (solid) and its extrapolation (dotted). The red symbols show the JWST objects as in Figure 7.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Full XRT band (0.3–10 keV) mosaic of the Galactic plane using an Aitoff projection in Galactic coordinates. The image covers the full footprint of DGPS Phase I. The pixel size is 4.″7 pix−1, and images have been smoothed with a Gaussian kernel (with FWHM of 3 pixels) to improve visual clarity. The image has been divided by the exposure map (Figure 2) in order to smooth out exposure-related background in the overlapping regions. The dominant sources of stray light at l ≈−25°, −20.°5, and 13.°5 are the LMXBs 4U 1624-49, 4U 1642-45, and GX 13+01.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Swift/XRT exposure map of the DGPS footprint. The ﹩4^{\prime} ﹩ overlap region between adjacent tiles is clearly demonstrated. A few tile positions were serendipitously observed twice, leading to a higher exposure (brighter regions). The median exposure across all pixels is 4.6 ks. The variation in exposure in the two observed regions of the GP is negligible.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Top: histogram of single-epoch Swift/XRT exposure time for all DGPS observations. Bottom: sky coverage as a cumulative function of the exposure time (corrected for vignetting and bad pixels) across the entire DGPS footprint after mosaicing all observations. The total sky coverage of the survey is 36 deg2. The median exposure time is 4.6 ks. The overlap regions between tiles lead to a higher exposure of up to 15–20 ks.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: The shaded blue regions show the line of sight of the DGPS footprint through the Milky Way’s disk. The background image is an illustration of the Milky Way, with credit to NASA/JPLCaltech/ESO/R. Hurt.