The IAC Stripe 82 Legacy Project: a wide-area survey for faint surface brightness astronomy

Fliri, J.; Trujillo, Ignacio

doi:10.1093/mnras/stv2686

Cited by 135 publications

(123 citation statements)

References 74 publications

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“…The multi-epoch data have been used to construct coadded images that can reach two magnitudes deeper than the SDSS single-epoch images (e.g. Annis et al 2014;Jiang et al 2014;Fliri & Trujillo 2016). Using these co-added data, we have found 12 z > 5.7 quasars in Stripe 82 (Jiang et al 2008(Jiang et al , 2009).…”

Section: Quasars In the Sdss Stripe 82mentioning

confidence: 99%

THE FINAL SDSS HIGH-REDSHIFT QUASAR SAMPLE OF 52 QUASARS AT z > 5.7

Jiang

McGreer

Fan

et al. 2016

ApJ

323

411

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We present the discovery of nine quasars at z ∼ 6 identified in the Sloan Digital Sky Survey (SDSS) imaging data. This completes our survey of z ∼ 6 quasars in the SDSS footprint. Our final sample consists of 52 quasars at 5.7 < z ≤ 6.4, including 29 quasars with z AB ≤ 20 mag selected from 11,240 deg 2 of the SDSS single-epoch imaging survey (the main survey), 10 quasars with 20 ≤ z AB ≤ 20.5 selected from 4223 deg 2 of the SDSS overlap regions (regions with two or more imaging scans), and 13 quasars down to z AB ≈ 22 mag from the 277 deg 2 in Stripe 82. They span a wide luminosity range of −29.0 ≤ M 1450 ≤ −24.5. This well-defined sample is used to derive the quasar luminosity function (QLF) at z ∼ 6. After combining our SDSS sample with two faint (M 1450 ≥ −23 mag) quasars from the literature, we obtain the parameters for a double power-law fit to the QLF. The bright-end slope β of the QLF is well constrained to be β = −2.8 ± 0.2. Due to the small number of low-luminosity quasars, the faint-end slope α and the characteristic magnitude M * 1450 are less well constrained, with α = −1.90The spatial density of luminous quasars, parametrized as ρ(M 1450 < −26, z) = ρ(z = 6) 10 k(z−6) , drops rapidly from z ∼ 5 to 6, with k = −0.72 ± 0.11. Based on our fitted QLF and assuming an IGM clumping factor of C = 3, we find that the observed quasar population cannot provide enough photons to ionize the z ∼ 6 IGM at ∼ 90% confidence. Quasars may still provide a significant fraction of the required photons, although much larger samples of faint quasars are needed for more stringent constraints on the quasar contribution to reionization.

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Section: Quasars In the Sdss Stripe 82mentioning

confidence: 99%

THE FINAL SDSS HIGH-REDSHIFT QUASAR SAMPLE OF 52 QUASARS AT z > 5.7

Jiang

McGreer

Fan

et al. 2016

ApJ

323

411

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“…In order to have a homogeneous dataset of dwarfs and UDGs both in depth and filter coverage, we use publicly available background-rectified imaging data in the g and r-bands of the deep IAC Stripe 82 Legacy Project 1 (hereafter IAC Stripe82, Fliri & Trujillo 2016;Román & Trujillo 2018). The UDGs are taken from Román & Trujillo (2017b) and Trujillo et al (2017).…”

Section: Data and Sample Selectionmentioning

confidence: 99%

Are ultra-diffuse galaxies Milky Way-sized?

Chamba

Trujillo

Knapen

2020

A&A

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Now almost 70 years since its introduction, the effective or half-light radius has become a very popular choice for characterising galaxy size. However, the effective radius measures the concentration of light within galaxies and thus does not capture the intuitive definition of size which is related to the edge or boundary of objects. For this reason, we aim to demonstrate the undesirable consequence of using the effective radius to draw conclusions about the nature of faint 'ultra-diffuse galaxies' (UDGs) when compared to dwarfs and Milky Way-like galaxies. Instead of the effective radius, we use a measure of galaxy size based on the location of the gas density threshold required for star formation. Compared to the effective radius, this physically motivated definition places the sizes much closer to the boundary of a galaxy. Therefore, considering the sizes and stellar mass density profiles of UDGs and regular dwarfs, we find that the UDGs have sizes that are within the size range of dwarfs. We also show that currently known UDGs do not have sizes comparable to Milky Way-like objects. We find that, on average, UDGs are ten times smaller in extension than Milky Way-like galaxies. These results show that the use of size estimators sensitive to the concentration of light can lead to misleading results.

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“…The IAC Stripe 82 Legacy Project (Fliri & Trujillo 2016) produces (co-)adds of the whole Stripe 82 data set using an automated (co-)addition pipeline. The pipeline queries all available data from the SDSS archive, aligns them photometrically and calibrates them to a common zero-point using calibration tables provided by SDSS for each image.…”

Section: Image Reduction and Calibrationmentioning

confidence: 99%

“…In the mean time a better PSF was determined using bright stars in addition to a very large number of faint stars (Fliri & Trujillo 2016). With this a new analysis of the outer parts of galaxies and the reality of the apparent extended stellar haloes is possible (Kelvin et al 2015).…”

Section: Possible Psf Effectsmentioning

confidence: 99%

Stellar disc truncations and extended haloes in face-on spiral galaxies

Peters

Kruit

Knapen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use data from the IAC Stripe82 Legacy Project to study the surface photometry of 22 nearby, face-on to moderately inclined spiral galaxies. The reprocessed and combined Stripe 82 g , r and i images allow us to probe the galaxy down to 29-30 r -magnitudes/arcsec 2 and thus reach into the very faint outskirts of the galaxies. Truncations are found in three galaxies. An additional 15 galaxies are found to have an apparent extended stellar halo. Simulations show that the scattering of light from the inner galaxy by the Point Spread Function (PSF) can produce faint structures resembling haloes, but this effect is insufficient to fully explain the observed haloes. The presence of these haloes and of truncations is mutually exclusive, and we argue that the presence of a stellar halo and/or light scattered by the PSF can hide truncations. Furthermore, we find that the onset of the stellar halo and the truncations scales tightly with galaxy size. Interestingly, the fraction of light does not correlate with dynamic mass. Nineteen galaxies are found to have breaks in their profiles, the radius of which also correlates with galaxy size.

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The IAC Stripe 82 Legacy Project: a wide-area survey for faint surface brightness astronomy

Cited by 135 publications

References 74 publications

THE FINAL SDSS HIGH-REDSHIFT QUASAR SAMPLE OF 52 QUASARS AT z > 5.7

THE FINAL SDSS HIGH-REDSHIFT QUASAR SAMPLE OF 52 QUASARS AT z > 5.7

Are ultra-diffuse galaxies Milky Way-sized?

Stellar disc truncations and extended haloes in face-on spiral galaxies

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