The miniJPAS survey: a preview of the Universe in 56 colours. (arXiv:2007.01910v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bonoli_S/0/1/0/all/0/1">S. Bonoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marin_Franch_A/0/1/0/all/0/1">A. Mar&#xed;n-Franch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Varela_J/0/1/0/all/0/1">J. Varela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramio_H/0/1/0/all/0/1">H. V&#xe1;zquez~Rami&#xf3;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abramo_L/0/1/0/all/0/1">L.R. Abramo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cenarro_A/0/1/0/all/0/1">A.J. Cenarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupke_R/0/1/0/all/0/1">R.A. Dupke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vilchez_J/0/1/0/all/0/1">J.M. V&#xed;lchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cristobal_Hornillos_D/0/1/0/all/0/1">D. Crist&#xf3;bal-Hornillos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delgado_R/0/1/0/all/0/1">R.M. Gonz&#xe1;lez Delgado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_Monteagudo_C/0/1/0/all/0/1">C. Hern&#xe1;ndez-Monteagudo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Sanjuan_C/0/1/0/all/0/1">C. L&#xf3;pez-Sanjuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muniesa_D/0/1/0/all/0/1">D.J. Muniesa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Civera_T/0/1/0/all/0/1">T. Civera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ederoclite_A/0/1/0/all/0/1">A. Ederoclite</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernan_Caballero_A/0/1/0/all/0/1">A. Hern&#xe1;n-Caballero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marra_V/0/1/0/all/0/1">V. Marra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baqui_P/0/1/0/all/0/1">P.O. Baqui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortesi_A/0/1/0/all/0/1">A. Cortesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cypriano_E/0/1/0/all/0/1">E.S. Cypriano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daflon_S/0/1/0/all/0/1">S. Daflon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amorim_A/0/1/0/all/0/1">A.L. de Amorim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_Garcia_L/0/1/0/all/0/1">L.A. D&#xed;az-Garc&#xed;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diego_J/0/1/0/all/0/1">J.M. Diego</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_Solaeche_G/0/1/0/all/0/1">G. Mart&#xed;nez-Solaeche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_E/0/1/0/all/0/1">E. P&#xe9;rez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Placco_V/0/1/0/all/0/1">V.M. Placco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prada_F/0/1/0/all/0/1">F. Prada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Queiroz_C/0/1/0/all/0/1">C.Queiroz</a> (148 additional authors not shown)

The Javalambre-Physics of the Accelerating Universe Astrophysical Survey
(J-PAS) will soon start to scan thousands of square degrees of the northern
extragalactic sky with a unique set of $56$ optical filters from a dedicated
$2.55$m telescope, JST, at the Javalambre Astrophysical Observatory. Before the
arrival of the final instrument (a 1.2 Gpixels, 4.2deg$^2$ field-of-view
camera), the JST was equipped with an interim camera (JPAS-Pathfinder),
composed of one CCD with a 0.3deg$^2$ field-of-view and resolution of 0.23
arcsec pixel$^{-1}$. To demonstrate the scientific potential of J-PAS, with the
JPAS-Pathfinder camera we carried out a survey on the AEGIS field (along the
Extended Groth Strip), dubbed miniJPAS. We observed a total of $sim 1$
deg$^2$, with the $56$ J-PAS filters, which include $54$ narrow band (NB,
$rm{FWHM} sim 145$Angstrom) and two broader filters extending to the UV and
the near-infrared, complemented by the $u,g,r,i$ SDSS broad band (BB) filters.
In this paper we present the miniJPAS data set, the details of the catalogues
and data access, and illustrate the scientific potential of our multi-band
data. The data surpass the target depths originally planned for J-PAS, reaching
$rm{mag}_{rm {AB}}$ between $sim 22$ and $23.5$ for the NB filters and up to
$24$ for the BB filters ($5sigma$ in a $3$~arcsec aperture). The miniJPAS
primary catalogue contains more than $64,000$ sources extracted in the $r$
detection band with forced photometry in all other bands. We estimate the
catalogue to be complete up to $r=23.6$ for point-like sources and up to
$r=22.7$ for extended sources. Photometric redshifts reach subpercent precision
for all sources up to $r=22.5$, and a precision of $sim 0.3$% for about half
of the sample. (Abridged)

The Javalambre-Physics of the Accelerating Universe Astrophysical Survey
(J-PAS) will soon start to scan thousands of square degrees of the northern
extragalactic sky with a unique set of $56$ optical filters from a dedicated
$2.55$m telescope, JST, at the Javalambre Astrophysical Observatory. Before the
arrival of the final instrument (a 1.2 Gpixels, 4.2deg$^2$ field-of-view
camera), the JST was equipped with an interim camera (JPAS-Pathfinder),
composed of one CCD with a 0.3deg$^2$ field-of-view and resolution of 0.23
arcsec pixel$^{-1}$. To demonstrate the scientific potential of J-PAS, with the
JPAS-Pathfinder camera we carried out a survey on the AEGIS field (along the
Extended Groth Strip), dubbed miniJPAS. We observed a total of $sim 1$
deg$^2$, with the $56$ J-PAS filters, which include $54$ narrow band (NB,
$rm{FWHM} sim 145$Angstrom) and two broader filters extending to the UV and
the near-infrared, complemented by the $u,g,r,i$ SDSS broad band (BB) filters.
In this paper we present the miniJPAS data set, the details of the catalogues
and data access, and illustrate the scientific potential of our multi-band
data. The data surpass the target depths originally planned for J-PAS, reaching
$rm{mag}_{rm {AB}}$ between $sim 22$ and $23.5$ for the NB filters and up to
$24$ for the BB filters ($5sigma$ in a $3$~arcsec aperture). The miniJPAS
primary catalogue contains more than $64,000$ sources extracted in the $r$
detection band with forced photometry in all other bands. We estimate the
catalogue to be complete up to $r=23.6$ for point-like sources and up to
$r=22.7$ for extended sources. Photometric redshifts reach subpercent precision
for all sources up to $r=22.5$, and a precision of $sim 0.3$% for about half
of the sample. (Abridged)

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