PDF (6M) - Isaac Newton Group of Telescopes - Instituto de ...

More documents

Recommendations

Info

Figure 35. Portions of the ISIS spectrum showing the OI, OI*, OI**, SiII, SiII* and SII lines. It is clearly visible that there are four discrete velocity components, with velocity differences of up to ~500 km s -1 . measurement of the neutral hydrogen column density and the metal content from weak, unsaturated singly-ionised sulphur (S II) lines, a metallicity of [S/H] = –0.84 ± 0.10, or ~0.14 times solar metallicity, was derived. This is in fact one of the highest metallicities measured from absorption lines at redshift around 4. From the very high column densities for the forbidden singly-ionised silicon (Si II*), and neutral oxygen (O I* and O I**) lines, the researchers infer very high densities in the system, significantly larger than 10 4 cm -3 . The high-resolution spectra also allow the astronomers to study the kinematics of the absorption systems. Several different, discrete velocity systems can be distinguished, with velocities of up to 500 km s -1 . Most surprisingly however, was the tentative detection of molecular hydrogen in the ISIS spectrum. This is the very first detection of molecular lines in an optical GRB afterglow spectrum. Especially remarkable is the fact that this possible detection has been achieved with a 4-metre telescope, proving that medium size telescopes can compete when response times are short. U AND B NUMBER COUNTS FROM THE GOYA SURVEY The Galaxy Origins and Young Assembly (GOYA) survey is designed to study the formation and evolution of galaxies with the aim of learning about the epoch and the Figure 36. Observations of the GOYA Survey in the GWS region over a DSS image. The 28 HST WFPC2 pointings defining the GWS in F606W and F814W are shown in gray, while J and Ks WHT INGRID fields are shown in white. The GWS runs diagonally across the wide 45'×45' field marked in black, which corresponds to the INT WFC field (U and B data). Numbers in black indicate positions and orientations of the four chips of WFC (figure from Eliche-Moral et al., 2006, ApJ, 639, 644). mechanisms by which galaxies assembled the bulk of their stars and acquired their present structure and dynamics. For this, a near-infrared/optical observational program using some of the most powerful ground-based telescopes and public data is being conducted to map 0.5 square degrees of high-latitude sky. As the main scientific motivation behind the design of EMIR (a NIR cryogenic multi-slit spectrograph for the 10.4m GTC at Observatorio del Roque de los Muchachos), GOYA emphasizes the use of near-infrared observations, which sample the optical rest-frame spectrum of galaxies at very high redshifts. The GOYA photometric survey is a multicolour survey in six broadband filters (U, B, V, I, J, K s ) with target depths of U=B=V=I=26 and J=K=22 (AB magnitudes). Its principal aim is to generate a galaxy database for sample selection and characterisation for subsequent NIR spectroscopy with EMIR. The U and B imaging came from observations carried out with the INT Wide Field Camera and covers the Groth- Westphal Strip (GWS). The GOYA Survey has also reduced and analysed data over this field in NIR filters from WHT INGRID (J and Ks) and in visible filters from HST WFPC2 (F606W and F814W). Originally, the GWS field 40 • ING BIENNIAL R EPORT 2006–2007
was defined as 28 HST WFPC2 pointings extended along a 45' strip. It has an area of ~150 arcmin 2 of sky. Compared to other existing optical-NIR surveys, GOYA offers a notable increase in the depth times area product in several filters, compiling complementary photometry in six optical-NIR bands and morphological and surface brightness information from high-resolution HST WFPC2 images. Counts were derived over the magnitude ranges 18.0
Page 1 and 2: I SAAC N EWTON G ROUP OF T ELESCOPE
Page 3 and 4: ISAAC NEWTON GROUP OF TELESCOPES Bi
Page 5 and 6: OF TELESCOPES The Isaac Newton Grou
Page 7 and 8: TABLE OF CONTENTS Foreword . . . .
Page 9 and 10: INTRODUCTION Welcome to the bi-annu
Page 11: Figure 2. Sequence of images of UGC
Page 15 and 16: observed the YORP effect in action
Page 17 and 18: Figure 7. Time-resolved spectroscop
Page 19 and 20: THE MEDIUM-RESOLUTION INT LIBRARY O
Page 21 and 22: Figure 11. Histograms showing the c
Page 23 and 24: BROWN DWARFS AND ISOLATED PLANETARY
Page 25 and 26: planets was named 'the 6th most imp
Page 27 and 28: Figure 22. Sample images from the M
Page 29 and 30: in its distance, And X appears to b
Page 31 and 32: small ellipticals in their central
Page 33 and 34: Figure 28. Left: I-band image with
Page 35 and 36: The number counts of kinematically
Page 37 and 38: Figure 32. Left: coverage of the la
Page 39: Figure 34. This INT Wide Field Came
Page 43 and 44: The European Galactic Plane Surveys
Page 45 and 46: of the giant (which will evolve tow
Page 47 and 48: has a large survey area and it was
Page 49 and 50: Chapter 2 OPERATION, MAINTENANCE AN
Page 51 and 52: Example results from the 2007 commi
Page 53 and 54: Figure 47. Two general-purpose L3CC
Page 55 and 56: Chapter 3 USE OF OBSERVING TIME AND
Page 57 and 58: Figure 55. Number of refereed paper
Page 59 and 60: Chapter 4 IN-HOUSE RESEARCH During
Page 61 and 62: using the stabilised spectrograph S
Page 63 and 64: Chapter 5 PUBLIC RELATIONS In 2006
Page 65 and 66: Appendix A THE ISAAC NEWTON GROUP O
Page 67 and 68: TELESCOPE TIME AND DATA OWNERSHIP T
Page 69 and 70: Appendix C STAFF ORGANISATION DIREC
Page 71 and 72: - Serra (Kapteyn), Stellar populati
Page 73 and 74: - Ward (Durham), The coronal lines
Page 75 and 76: - Southworth (Warwick), The ultra-l
Page 77 and 78: - Kurtz (Lancashire), A test of a n
Page 79 and 80: Appendix E ING BIBLIOGRAPHY Below a
Page 81 and 82: 37. B. T. Gänsicke, T. R. Marsh, J
Page 83 and 84: 87. O. K. Sil'chenko, A. V. Moiseev
Page 85 and 86: 30. B. Gänsicke, T. R. Marsh, J. S
Page 87 and 88: 2. G. Anglada, R. López, R. Estale
Page 89 and 90: 52. E. Noordermeer, J. M. van der H
Page 91 and 92:
13. A. Collier Cameron, D. M. Wilso
Page 93 and 94:
64. D. J. B. Smith, M. J. Jarvis, 2
Page 95 and 96:
21. Dufton, P. L., Ryans, R. S. I.,
Page 97 and 98:
Wheatley, P. J., Wilson, D. M., 200
Page 99 and 100:
Appendix G SEMINARS Date Title Spea
Page 101 and 102:
Appendix I COMMITTEE MEMBERSHIP ING
Page 103 and 104:
Appendix J ADDRESSES AND CONTACTS I
Page 105:
LIRIS LJMU MARTINI MES Mem Soc Astr
show all

PDF (6M) - Isaac Newton Group of Telescopes - Instituto de ...

Create successful ePaper yourself

Delete template?

Save as template?