. . . . . . . . . "aa20838-12" . . . "Context. A gas giant planet has previously been directly seen orbiting at 8-10 AU within the debris disk of the ~12 Myr old star \u03B2 Pictoris. The \u03B2 Pictoris system offers the rare opportunity of both studying the physical and atmospheric properties of an exoplanet placed on a wide orbit and establishing its formation scenario. Aims. We aim to build the 1-5 \u03BCm spectral energy distribution of the planet for the first time. Our goal is to provide secure and accurate constraints on its physical and chemical properties. Methods. We obtained J (1.265 \u03BCm), H (1.66 \u03BCm), and M\u2032 (4.78 \u03BCm) band angular differential imaging of the system between 2011 and 2012. We used Markov chain Monte Carlo simulations of the astrometric data to revise constraints on the orbital parameters of the planet. Photometric measurements were compared to those of ultra-cool dwarfs and young companions. They were combined with existing photometry (2.18, 3.80, and 4.05 \u03BCm) and compared to predictions from 7 PHOENIX-based atmospheric models in order to derive the atmospheric parameters ( Teff, log g) of \u03B2 Pictoris b. Predicted properties from (\u201Chot-start\u201D, \u201Ccold-start\u201D, and \u201Cwarm start\u201D) evolutionary models were compared to independent constraints on the mass of \u03B2 Pictoris b. We used planet-population synthesis models following the core-accretion paradigm to discuss the planet\u2019s possible origin. Results. We detect the planetary companion in our four-epoch observations. We estimate J\u00A0=\u00A014.0\u00A0\u00B1\u00A00.3, H\u00A0=\u00A013.5\u00A0\u00B1\u00A00.2, and M\u2032\u00A0=\u00A011.0\u00A0\u00B1\u00A00.3 mag. Our new astrometry consolidates previous semi-major axis (8-10 AU) and excentricity ( e\u00A0\u2264\u00A00.15) estimates of the planet. The location of \u03B2 Pictoris b in color-magnitude diagrams suggests it has spectroscopic properties similar to L0-L4 dwarfs. This enables one to derive Log 10 ( L\u00A0/\u00A0 L\u2299)\u00A0= \u2212\u00A03.87\u00A0\u00B1\u00A00.08 for the companion. The analysis with atmospheric models reveals that the planet has a dusty atmosphere with Teff\u00A0=\u00A01700\u00A0\u00B1\u00A0100K and log \u00A0 g\u00A0=\u00A04.0\u00A0\u00B1\u00A00.5. \u201CHot-start\u201D evolutionary models give a new mass of 10 -2+3MJup from Teff and 9 -2+3MJup from luminosity. Predictions of \u201Ccold-start\u201D models are still inconsistent with independent constraints on the planet mass. \u201CWarm-start\u201D models constrain the mass to M\u00A0\u2265\u00A06 MJup and the initial entropies to values ( Sinit\u00A0\u2265\u00A09.3 Kb\u00A0/\u00A0baryon) midway between those considered for cold/hot-start models, but probably closer to those of hot-start models."@en . . . "ESO" . . . . . . . . . . . . . "2013"^^ . . . . . . "\u00A9 ESO, 2013" . . . . . . "2013"^^ . "The near-infrared spectral energy distribution of \u03B2 Pictoris b"@en . . . .