Remember Me
Or use your Academic/Social account:


Or use your Academic/Social account:


You have just completed your registration at OpenAire.

Before you can login to the site, you will need to activate your account. An e-mail will be sent to you with the proper instructions.


Please note that this site is currently undergoing Beta testing.
Any new content you create is not guaranteed to be present to the final version of the site upon release.

Thank you for your patience,
OpenAire Dev Team.

Close This Message


Verify Password:
Verify E-mail:
*All Fields Are Required.
Please Verify You Are Human:
fbtwitterlinkedinvimeoflicker grey 14rssslideshare1
Fomalont, EB; Vlahakis, C; Corder, S; Remijan, A; Barkats, D; Lucas, R; Hunter, TR; Brogan, CL; Asaki, Y; Matsushita, S; Dent, WRF; Hills, RE; Phillips, N; Richards, AMS; Cox, P; Amestica, R; Broguiere, D; Cotton, W; Hales, AS; Hiriart, R; Hirota, A; Hodge, JA; Impellizzeri, CMV; Kern, J; Kneissl, R; Liuzzo, E; Marcelino, N; Marson, R; Mignano, A; Nakanishi, K ... view all 249 authors View less authors
Languages: English
Types: Article
Subjects: QB
A major goal of the Atacama Large Millimeter/submillimeter Array (ALMA) is to make accurate images with resolutions of tens of milliarcseconds, which at submillimeter (submm) wavelengths requires baselines up to ∼15 km. To develop and test this capability, a Long Baseline Campaign (LBC) was carried out from 2014 September to late November, culminating in end-to-end observations, calibrations, and imaging of selected Science Verification (SV) targets. This paper presents an overview of the campaign and its main results, including an investigation of the short-term coherence properties and systematic phase errors over the long baselines at the ALMA site, a summary of the SV targets and observations, and recommendations for science observing strategies at long baselines. Deep ALMA images of the quasar 3C 138 at 97 and 241 GHz are also compared to VLA 43 GHz results, demonstrating an agreement at a level of a few percent. As a result of the extensive program of LBC testing, the highly successful SV imaging at long baselines achieved angular resolutions as fine as 19 mas at ∼350 GHz. Observing with ALMA on baselines of up to 15 km is now possible, and opens up new parameter space for submm astronomy. .
  • The results below are discovered through our pilot algorithms. Let us know how we are doing!

    • ALMA Partnership et al., 2015a, ApJL, in press (arXiv:1503.02650)
    • ALMA Partnership et al., 2015b, ApJL, in press (arXiv:1503.02649)
    • ALMA Partnership et al., 2015c, ApJL, in press (arXiv:1503.02652)
    • Asaki, Y et al, Proc. SPIE, 9145, 91454K
    • Beasley, A. J. & Conway, J. E. 1995, ASP Conf. Ser. 82, Very Long Base-line Interferometry and the VLBA, ed. J. A. Zensus, P. J. Diamond, & P. J. Napier (San Francisco: ASP), 328 R., Pardo, J., & Roche, J.-C. 2011, Astronomical Data Analysis Software and Systems XX, 442, 277
    • Carilli, C.L. & Holdaway, M.A. 1999, Radio Science, 34, 817
    • Cotton W.D. et al. 1997, A&A, 325, 493
    • Cotton W.D. et al. 2003, A&A, 406, 43
    • Cotton, W. D. 2008, PASP, 120,439.
    • Emrich, A., Andersson, S., Wannerbratt, M., et al. 2009, Twentieth International Symposium on Space Terahertz Technology, 174
    • Fomalont, E. & Perley, R., in Synthesis Imaging in Radio Astronomy II, ASP Conference Series, 180, 1999, ed (Taylor, Carilli and Perley), p.90
    • Fomalont, E. & Kopeikin, S 2002 in6th European VLBI Network Symposium on New Developments in VLBI Science and Technology, held in Bonn, June 25th-28th 2002, proceedings edited by E. Ros, R. W. Porcas, A. P. Lobanov, and J. A. Zensus, published by the Max-Planck-Institut für Radioastronomie (Bonn). p. 53.
    • Lestrade J.-F. 2008, in IAU Symp. No. 248. A Giant Step: from Milli- to Micro-arcsecond Astrometry, ed. W. J. Jin, I. Platais & M. A. C. Perryman (CUP) 170
    • Marson, R., Kern, J., Farris, A., & Hiriart, R. 2008, Proc. SPIE, 7019, 701905
    • Massardi, M, Ekers, R., Murphy, T, et al, 2011, MNRAS, 412, 318
    • Matsushita S. et al. 1999, PASJ, 51, 603
    • Matsushita S., Asaki, Y., Kawabe, R, Fomalont, E., Barkats, D. & Corder, S., 2014, Proc. SPIE, 9145, 914531l
    • Nikolic, B., Bolton, R. C., Graves, S. F., Hills, R. E., & Richer, J. S. 2013, A&A, 552, AA104
    • Richards, M.A. 2003 IEEE Signal Processing Letters, 10, 208
    • Reid, M. J., & Honma, M. 2014, ARA&A, 52, 339 R. C., Kirkland, M. W., Kao, C.-Y. J.,& Jacobson, A. R. 1999, J. Geophys. Res., 104, 16729
    • Interferometry and Synthesis in Radio Astronomy, 2001, Second Ed, A. Richard Thompson, James, M. Moran, George W Swenson, Jr, John Wiley and Sons, New York, p512.
  • No related research data.
  • No similar publications.

Share - Bookmark

Cite this article