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Follow-up observations performed in late 2009 and early 2010 using the same instrument recovered and confirmed the planet, but on the opposite side of the star. These findings were published in the journal ''[[Science (journal)|Science]]''<ref name="LagrangeBonnefoy2010">{{cite journal |last1=Lagrange |first1=A.- M. |last2=Bonnefoy |first2=M. |last3=Chauvin |first3=G. |last4=Apai |first4=D. |last5=Ehrenreich |first5=D. |last6=Boccaletti |first6=A. |last7=Gratadour |first7=D. |last8=Rouan |first8=D. |last9=Mouillet |first9=D. |last10=Lacour |first10=S. |last11=Kasper |first11=M. |title=A Giant Planet Imaged in the Disk of the Young Star Pictoris |journal=Science |volume=329 |issue=5987 |year=2010 |pages=57–59 |issn=0036-8075 |doi=10.1126/science.1187187|arxiv = 1006.3314 |bibcode = 2010Sci...329...57L |pmid=20538914|s2cid=5427102 }}</ref> and represented the closest orbiting planet to its star ever imaged. Observations performed in late 2010 and early 2011 allowed scientists to establish an [[Orbital inclination|inclination]] angle of the planet's orbit of 88.5 degrees, nearly edge-on. The location of the planet was found to be approximately 3.5 to 4 degrees tilted from the main disk in this system, indicating that the planet is aligned with the warped inner disk in the Beta Pictoris system.<ref name="ChauvinLagrange2012">{{cite journal|last1=Chauvin|first1=G.|last2=Lagrange|first2=A.-M.|last3=Beust|first3=H.|last4=Bonnefoy|first4=M.|last5=Boccaletti|first5=A.|last6=Apai|first6=D.|last7=Allard|first7=F.|last8=Ehrenreich|first8=D.|last9=Girard|first9=J. H. V.|last10=Mouillet|first10=D.|last11=Rouan|first11=D.|title=Orbital characterization of the β Pictoris b giant planet|journal=Astronomy & Astrophysics|volume=542|year=2012|pages=A41|issn=0004-6361|doi=10.1051/0004-6361/201118346|arxiv = 1202.2655 |bibcode = 2012A&A...542A..41C |s2cid=62806093}}</ref>
The first study of the spectral energy distribution of the planet was published in July 2013.<ref name="BonnefoyBoccaletti2013">{{cite journal |last1=Bonnefoy |first1=M. |last2=Boccaletti |first2=A. |last3=Lagrange |first3=A.-M. |last4=Allard |first4=F. |last5=Mordasini |first5=C. |last6=Beust |first6=H. |last7=Chauvin |first7=G. |last8=Girard |first8=J. H. V. |last9=Homeier |first9=D. |last10=Apai |first10=D. |last11=Lacour |first11=S. |last12=Rouan |first12=D. |title=The near-infrared spectral energy distribution ofβPictoris b |journal=Astronomy & Astrophysics |volume=555 |year=2013 |pages=A107 |issn=0004-6361 |doi=10.1051/0004-6361/201220838|arxiv = 1302.1160 |bibcode = 2013A&A...555A.107B |s2cid=54014134 }}</ref> This study shows detections at 1.265, 1.66, 2.18, 3.80, 4.05 and 4.78 [[Micrometre|
In 2015, a short video was made from direct images of Beta Pictoris b taken by the [[Gemini Planet Imager]] over the course of about two years showing a time-lapse of the planet orbiting around its parent star.<ref>{{Cite web|title = Watching an exoplanet in motion around a distant star {{!}} Astronomy Now|url = http://astronomynow.com/2015/09/17/watching-an-exoplanet-in-motion-around-a-distant-star/|access-date = 2015-09-29|first = Astronomy|last = Now}}</ref> It may have been responsible for a [[Planetary transit|transit]]-like event observed in 1981.
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