Overview of the DESI Legacy Imaging Surveys

Dey, Arjun; Schlegel, David J.; Lang, Dustin; Blum, Robert; Burleigh, Kaylan; Fan, Xiaohui; Findlay, Joseph R.; Finkbeiner, Doug; Herrera, David; Juneau, Stéphanie; Landriau, Martin; Levi, M. E.; McGreer, Ian D.; Meisner, Aaron M.; Myers, Adam D.; Moustakas, John; Nugent, P.; Patej, Anna; Schlafly, Edward F.; Walker, A. R.; Valdés, Francisco; Weaver, B. A.; Zou, Christophe Yeche Hu; Zhou, Xu; Abareshi, Behzad; Abbott, T. M. C.; Abolfathi, Bela; Aguilera, C.; Alam, Shadab; Allen, Lori; Álvarez, Amaury Cabarcas; Annis, James; Ansarinejad, Behzad; Aubert, M; Beechert, Jacqueline; Bell, Eric F.; BenZvi, S.; Beutler, Florian; Bielby, R. M.; Bolton, A.; Buckley-Geer, Cesar Briceno Elizabeth J.; Butler, Karen A.; Calamida, A.; Carlberg, R. G.; Carter, Paul; Casas, R.; Castander, F. J.; Choi, Yumi; Comparat, Johan; Cukanovaite, E.; Delubac, Timothée; DeVries, Kaitlin; Dey, Sharmila; Dhungana, G.; Dickinson, Mark; Ding, Zhejie; Donaldson, John B.; Duan, Yutong; Duckworth, Christopher; Eftekharzadeh, Sarah; Eisenstein, Daniel J.; Etourneau, Thomas; Fagrelius, Parker; Farihi, Jay; Fitzpatrick, Mike; Font-Ribera, Andreu; Fulmer, Leah; Gänsicke, B. T.; Gaztañaga, E.; George, Koshy; Gerdes, D. W.; Gontcho, Satya Gontcho A; Gorgoni, Claudio; Green, Gregory; Guy, J.; Harmer, Dianne; Hernández, M. S.; Honscheid, K.; Lijuan, Lijuan; Huang, Biao; James, D. J.; Jannuzi, Buell T.; Jiang, Linhua; Joyce, Richard; Karcher, A.; Karkar, S.; Kehoe, R.; Kneib, Jean-Paul; Kueter-Young, Andrea; Lan, Ting-Wen; Lauer, Tod R.; Guillou, L. Le; Suu, A. Le van; Lee, Jaehyeon; Lesser, Michael P.; Perreault-Levasseur, Laurence; Li, Ting S.; Mann, Justin L.; Marshall, Bob; Martı́nez-Vázquez, C. E.; Martini, Paul; Bourboux, Hélion du Mas des; McManus, Sean; Meier, Tobias G.; Ménard, Brice; Metcalfe, N.; Muñoz‐Gutiérrez, Andrea; Najita, J.; Napier, Kevin; Narayan, Gautham; Newman, Jeffrey A.; Nie, Jundan; Nord, B.; Norman, Dara; Olsen, Knut; Paat, Anthony; Palanque-Delabrouille, N.; Peng, Xiyan; Poppett, Claire; Poremba, Megan R.; Prakash, Abhishek; Rabinowitz, D.; Raichoor, Anand; Rezaie, Mehdi; Robertson, Amy; Roe, Natalie A.; Ross, Ashley J.; Ross, Nicholas P.; Rudnick, Gregory; Safonova, Sasha; Saha, Abhijit; Sánchez, Francisco Javier Martín; Savary, E.; Schweiker, Heidi; Scott, A.; Seo, Hee-Jong; Shan, Huanyuan; Silva, David R.; Slepian, Zachary; Soto, Christian; Sprayberry, David; Staten, Ryan; Stillman, Coley M.; Stupak, Robert J.; Summers, D. L.; Tie, Suk Sien; Tirado, H.; Vargas-Magaña, Mariana; Vivas, A. Katherina; Wechsler, Risa H.; Williams, Doug; Yang, Jinyi; Yang, Qian; Yapici, T.; Zaritsky, Dennis; Zenteno, A.; Zhang, Kai; Zhang, Tianmeng; Zhou, Rongpu; Zhang, Zhimin

doi:10.3847/1538-3881/ab089d

Cited by 1,074 publications

(785 citation statements)

References 94 publications

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“…As a quality check, we only kept in the subsequent analysis those sources with morphological model 'psf' (stellar point sources), which resulted to have errors in the PSF g magnitude and g − r color less than 0.04 and 0.07 mag, respectively. These upper limits for the photometric errors allow us to deal with a photometry completeness nearly 100 per cent at g ≤ 23.0 mag for the outer cluster regions, where crowding effects are negligible (Dey et al 2019).…”

Section: Data Handingmentioning

confidence: 99%

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Pal 13: its moderately extended low-density halo and its accretion history

Piatti

Fernández-Trincado

2020

A&A

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We present results on the basis of Dark Energy Camera Legacy Survey (DECaLS) DR8 astrometric and photometric data sets of the Milky Way globular cluster Pal 13. Because of its relative small size and mass, there has not been yet a general consensus about the existence of extra-tidal structures around it. While some previous results claim for the absence of such features, others have shown that the cluster is under the effects of tidal stripping. From DECaLS g, r magnitudes of stars placed along the cluster Main Sequence in the color-magnitude diagram -previously corrected by interstellar reddening-, we built the cluster stellar density map. The resulting density map shows nearly smooth contours around Pal 13 out to ≈ 1.6 times the most recent estimate of its Jacobi radius, derived by taking into account its variation along its orbital motion. This outcome favors the presence of stars escaping the cluster, a phenomenon frequently seen in globular clusters that have crossed the Milky Way disc a comparable large number of times. Particularly, the orbital high eccentricity and large inclination angle of this accreted globular cluster could have been responsible for the relatively large amount of cluster mass lost.

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Section: Data Handingmentioning

confidence: 99%

“…We here exploit the Dark Energy Camera Legacy Survey (DECaLS, Dey et al 2019) in order to address the issue about the existence of extra-tidal features around Pal 13. Section 2 describes the retrieved data sets, while in Section 3 we deal with the construction of the intrinsic cluster stellar density map.…”

Section: Introductionmentioning

confidence: 99%

Pal 13: its moderately extended low-density halo and its accretion history

Piatti

Fernández-Trincado

2020

A&A

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“…In addition to these galaxies, some of our host galaxies can still contain a small fraction of young stellar component. To check this, when available, we have examined the level of young star contamination in our host sample by using the NUV -, r-, and W 3-band images from GALEX (Martin et al 2005), SDSS (Abolfathi et al 2018) or DESI Legacy Imaging Surveys (Dey et al 2019), and unWISE (Lang 2014) databases. We find that three galaxies (hosts of SN 2002G, SN 2007cp, and SN 2007R) have very large excess emissions both in NUV and W 3, clearly separated from other host galaxies (see Figure 8), indicating a significant contamination from ongoing or recent star formation.…”

Section: Correlation Between Population Age and Hubble Residual Of Sn Iamentioning

confidence: 99%

Early-type Host Galaxies of Type Ia Supernovae. II. Evidence for Luminosity Evolution in Supernova Cosmology

Kang

Lee

Kim

et al. 2020

ApJ

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The most direct and strongest evidence for the presence of dark energy is provided by the measurement of galaxy distances using SNe Ia. This result is based on the assumption that the corrected brightness of SN Ia through the empirical standardization would not evolve with look-back time. Recent studies have shown, however, that the standardized brightness of SN Ia is correlated with host morphology, host mass, and local star formation rate (SFR), suggesting a possible correlation with stellar population property. To understand the origin of these correlations, we have continued our spectroscopic observations to cover most of the reported nearby early-type host galaxies. From high-quality (signal-to-noise ratio ∼175) spectra, we obtained the most direct and reliable estimates of population age and metallicity for these host galaxies.We find a significant correlation between SN luminosity (after the standardization) and stellar population age at a 99.5% confidence level. As such, this is the most direct and stringent test ever made for the luminosity evolution of SN Ia. Based on this result, we further show that the previously reported correlations with host morphology, host mass, and local SFR are most likely originated from the difference in population age.This indicates that the light-curve fitters used by the SNe Ia community are not quite capable of correcting for the population age effect, which would inevitably cause a serious systematic bias with look-back time. Notably, taken at face values, most of the Hubble residual used in the discovery of the dark energy appears to be affected by the luminosity evolution. ). According to the analysis by Childress et al. (2014), the difference in the mean age of SN progenitors between z = 0 and 1.0 is predicted to be ∼5.3 Gyr (see also Section 4 below). It is therefore possible that SNe at high redshift are fainter (after the standardization) than the value expected from the model without the dark energy, not because of the dark energy, but mostly because of the luminosity evolution. Careful investigation of this possible systematic bias with redshift is particularly important because the dimming of SNe is only ∼0.2 mag (∼20% in brightness) with respect to a cosmological model without dark energy (Ω M = 0.27, Ω Λ = 0.00; Hicken et al. 2009).Nevertheless, to test the effect of luminosity evolution, in the discovery papers, Riess et al. (1998), Schmidt et al. (1998), and Perlmutter et al. (1999 only used morphological classification of host galaxies in the local universe as a proxy for stellar population age. Because of apparently very small difference in the standardized brightness between SNe Ia in the early-type and late-type host galaxies, they concluded that the luminosity evolution is negligible in SN cosmology. Later analysis based on a larger sample by Hicken et al. (2009), however, found a systematic difference of ∼0.14 mag between the very early-and very late-type galaxies (see also Suzuki et al. 2012). Recent investigations of host galaxies further found a co...

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“…This visual inspection results in a sample of 425 potential low surface brightness, "ultra diffuse" sources. While deeper imaging surveys are becoming available (e.g., Chambers et al 2016;Dey et al 2019), developing analogous extraction and surface brightness profile fitting tools for ALFALFA sources in those datasets is complex and the subject of other ongoing work (Greco et al 2018.…”

Section: Huds Sample Selection Criteriamentioning

confidence: 99%

The environment of H i-bearing ultra-diffuse galaxies in the ALFALFA survey

Janowiecki

Jones

Leisman

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We explore the environment of 252 H -bearing Ultra Diffuse Galaxies (HUDs) from the 100% ALFALFA survey catalog in an attempt to constrain their formation mechanism. We select sources from ALFALFA with surface brightnesses, magnitudes, and radii consistent with other samples of Ultra Diffuse Galaxies (UDGs), without restrictions on their isolation or environment, more than doubling the previously reported ALFALFA sample. We quantify the galactic environment of HUDs using several metrics, including n-th nearest neighbour, tidal influence, membership in a group/cluster, and distance from nearest group/cluster or filament. We find that that HUDs inhabit the same environments as other samples of Hselected galaxies and that they show no environmental preference in any metric. We suggest that these results are consistent with a picture of the extreme properties of HUDs being driven by internal mechanisms and that they are largely unperturbed by environmental impacts. While environmental effects may be necessary to convert HUDs into gas-poor cluster UDGs, these effects are not required for diffuse galaxies to exist in the first place.These results have demonstrated that H content is clearly tied to both internal and environmental aspects of galaxy formation, however to date there has been no such study specific to H -bearing Ultra Diffuse galaxies (HUDs), thus whether or not their extreme

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Overview of the DESI Legacy Imaging Surveys

Cited by 1,074 publications

References 94 publications

Pal 13: its moderately extended low-density halo and its accretion history

Pal 13: its moderately extended low-density halo and its accretion history

Early-type Host Galaxies of Type Ia Supernovae. II. Evidence for Luminosity Evolution in Supernova Cosmology

The environment of H i-bearing ultra-diffuse galaxies in the ALFALFA survey

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