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In recent years, some evidence has emerged of small temporal and also spatial variations in <jats:italic>\u03b1<\/jats:italic> on cosmological scales which may reach a fractional level of \u2248 10 ppm (parts per million). We are conducting a Large Programme of observations with the Very Large Telescope's Ultraviolet and Visual Echelle Spectrograph (UVES), and are obtaining high\u2010resolution (<jats:italic>R<\/jats:italic> \u2248 60000) and high signal\u2010to\u2010noise ratio (S\/N \u2248 100) spectra calibrated specifically to study the variations of the fundamental constants. We here provide a general overview of the Large Programme and report on the first results for these two constants, discussed in detail in Molaro et al. (2013) and Rahmani et al. (2013). A stringent bound for \u0394<jats:italic>\u03b1<\/jats:italic> \/<jats:italic>\u03b1<\/jats:italic> is obtained for the absorber at <jats:italic>z<\/jats:italic><jats:sub>abs<\/jats:sub> = 1.6919 towards HE 2217\u20102818. The absorption profile is complex with several very narrow features, and is modeled with 32 velocity components. The relative variation in <jats:italic>\u03b1<\/jats:italic> in this system is +1.3 \u00b1 2.4<jats:sub>stat<\/jats:sub> \u00b1 1.0<jats:sub>sys<\/jats:sub> ppm if Al II <jats:italic>\u03bb<\/jats:italic> 1670 \u00c5 and three FeII transitions are used, and +1.1 \u00b1 2.6<jats:sub>stat<\/jats:sub> ppm in a slightly different analysis with only FeII transitions used. This is one of the tightest bounds on <jats:italic>\u03b1<\/jats:italic> \u2010variation from an individual absorber and reveals no evidence for variation in <jats:italic>\u03b1<\/jats:italic> at the 3\u2010ppm precision level (1<jats:italic>\u03c3<\/jats:italic> confidence). The expectation at this sky position of the recently\u2010reported dipolar variation of <jats:italic>\u03b1<\/jats:italic> is (3.2\u20135.4) \u00b1 1.7 ppm depending on dipole model used and this constraint of \u0394<jats:italic>\u03b1<\/jats:italic> \/<jats:italic>\u03b1<\/jats:italic> at face value is not supporting this expectation but not inconsistent with it at the 3<jats:italic>\u03c3<\/jats:italic> level. For the proton\u2010to\u2010electron mass ratio the analysis of the H<jats:sub>2<\/jats:sub> absorption lines of the <jats:italic>z<\/jats:italic><jats:sub>abs<\/jats:sub> \u2248 2.4018 damped Ly<jats:italic>\u03b1<\/jats:italic> system towards HE 0027\u20131836 provides \u0394<jats:italic>\u03bc<\/jats:italic> \/<jats:italic>\u03bc<\/jats:italic> = (\u20137.6 \u00b1 8.1<jats:sub>stat<\/jats:sub> \u00b1 6.3<jats:sub>sys<\/jats:sub>) ppm which is also consistent with a null variation. The cross\u2010correlation analysis between individual exposures taken over three years and comparison with almost simultaneous asteroid observations revealed the presence of a possible wavelength dependent velocity drift as well as of inter\u2010order distortions which probably dominate the systematic error and are a significant obstacle to achieve more accurate measurements. (\u00a9 2014 WILEY\u2010VCH Verlag GmbH &amp; Co. KGaA, Weinheim)<\/jats:p>","DOI":"10.1002\/asna.201312005","type":"journal-article","created":{"date-parts":[[2014,10,15]],"date-time":"2014-10-15T15:37:19Z","timestamp":1413387439000},"page":"83-91","source":"Crossref","is-referenced-by-count":24,"title":["Fundamental constants and high\u2010resolution spectroscopy"],"prefix":"10.1002","volume":"335","author":[{"given":"P.","family":"Bonifacio","sequence":"first","affiliation":[]},{"given":"H.","family":"Rahmani","sequence":"additional","affiliation":[]},{"given":"J.B.","family":"Whitmore","sequence":"additional","affiliation":[]},{"given":"M.","family":"Wendt","sequence":"additional","affiliation":[]},{"given":"M.","family":"Centurion","sequence":"additional","affiliation":[]},{"given":"P.","family":"Molaro","sequence":"additional","affiliation":[]},{"given":"R.","family":"Srianand","sequence":"additional","affiliation":[]},{"given":"M.T.","family":"Murphy","sequence":"additional","affiliation":[]},{"given":"P.","family":"Petitjean","sequence":"additional","affiliation":[]},{"given":"I.I.","family":"Agafonova","sequence":"additional","affiliation":[]},{"given":"S.","family":"D'Odorico","sequence":"additional","affiliation":[]},{"given":"T.M.","family":"Evans","sequence":"additional","affiliation":[]},{"given":"S.A.","family":"Levshakov","sequence":"additional","affiliation":[]},{"given":"S.","family":"Lopez","sequence":"additional","affiliation":[]},{"given":"C.J.A.P.","family":"Martins","sequence":"additional","affiliation":[]},{"given":"D.","family":"Reimers","sequence":"additional","affiliation":[]},{"given":"G.","family":"Vladilo","sequence":"additional","affiliation":[]}],"member":"311","published-online":{"date-parts":[[2014,1,10]]},"reference":[{"key":"e_1_2_1_2_1","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevD.86.063515"},{"key":"e_1_2_1_3_1","doi-asserted-by":"publisher","DOI":"10.1126\/science.1224898"},{"key":"e_1_2_1_4_1","doi-asserted-by":"publisher","DOI":"10.1086\/180042"},{"key":"e_1_2_1_5_1","doi-asserted-by":"publisher","DOI":"10.1051\/0004-6361:200809629"},{"key":"e_1_2_1_6_1","doi-asserted-by":"publisher","DOI":"10.1051\/0004-6361:20054584"},{"key":"e_1_2_1_7_1","doi-asserted-by":"publisher","DOI":"10.1086\/176422"},{"key":"e_1_2_1_8_1","doi-asserted-by":"publisher","DOI":"10.1038\/139323a0"},{"key":"e_1_2_1_9_1","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevLett.82.888"},{"key":"e_1_2_1_10_1","doi-asserted-by":"publisher","DOI":"10.1088\/0004-637X\/708\/1\/158"},{"key":"e_1_2_1_11_1","doi-asserted-by":"publisher","DOI":"10.1051\/0004-6361\/200811475"},{"key":"e_1_2_1_12_1","doi-asserted-by":"publisher","DOI":"10.1088\/2041-8205\/728\/1\/L12"},{"key":"e_1_2_1_13_1","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevLett.101.251304"},{"key":"e_1_2_1_14_1","doi-asserted-by":"publisher","DOI":"10.1111\/j.1365-2966.2011.19460.x"},{"key":"e_1_2_1_15_1","doi-asserted-by":"publisher","DOI":"10.1111\/j.1365-2966.2012.20852.x"},{"key":"e_1_2_1_16_1","first-page":"189","volume":"8","author":"Kurucz R. 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