CMS distributed computing workflow experience

Adelman-McCarthy, Jennifer K.; Gutsche, O.; Haas, Jeffrey J.D.; Prosper, H.; Gómez-Ceballos, G.; Hahn, K. A.; Klute, M.; Mohapatra, A.; Kçira, D.; Caudron, J.; Liao, J.; Pin, A.; Schul, N.; Lentdecker, G. De; Mccartin, J.; Vanelderen, L.; Janssen, X.; Tsyganov, A.; Barge, D.; Lahiff, Andrew

doi:10.1088/1742-6596/331/7/072019

Cited by 3 publications

(3 citation statements)

References 4 publications

(6 reference statements)

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“…The telescope was defocused so that the FWHM of the stellar PSF is about 10 pixels, or ∼15 ′′ , for the same purpose as the ISLE observations. We note that the contamination light from objects surrounding the target star is negligible because there is no object brighter than 20 and 16 magnitudes in any band within 10 ′′ and 20 ′′ , respectively, from GJ3470 in the Sloan Digital Sky Survey (SDSS) photometric catalog (Adelman- McCarthy & et al 2011). We started the MITSuME observations about 35 minutes behind the ISLE observations.…”

Section: Mitsume Optical Observationsmentioning

confidence: 99%

OPTICAL-TO-NEAR-INFRARED SIMULTANEOUS OBSERVATIONS FOR THE HOT URANUS GJ3470b: A HINT OF A CLOUD-FREE ATMOSPHERE

Fukui¹,

Narita²,

Kurosaki³

et al. 2013

ApJ

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We present optical (g ′ , R c , and I c ) to near-infrared (J) simultaneous photometric observations for a primary transit of GJ3470b, a Uranus-mass transiting planet around a nearby M dwarf, by using the 50-cm MITSuME telescope and the 188-cm telescope both at Okayama Astrophysical Observatory. From these data, we derive the planetary mass, radius, and density as 14.1 ± 1.3 M ⊕ , 4.32 +0.21 −0.10 R ⊕ , and 0.94 ± 0.12 g cm −3 , respectively, thus confirming the low density that was reported by Demory et al. based on the Spitzer/IRAC 4.5-µm photometry (0.72 +0.13 −0.12 g cm −3 ). Although the planetary radius is about 10% smaller than that reported by Demory et al., this difference does not alter their conclusion that the planet possesses a hydrogen-rich envelope whose mass is approximately 10% of the planetary total mass. On the other hand, we find that the planet-to-star radius ratio (R p /R s ) in the J band (0.07577 +0.00072 −0.00075 ) is smaller than that in the I c (0.0802 ± 0.0013) and 4.5-µm (0.07806 +0.00052 −0.00054 ) bands by 5.8% ± 2.0% and 2.9% ± 1.1%, respectively. A plausible explanation for the differences is that the planetary atmospheric opacity varies with wavelength due to absorption and/or scattering by atmospheric molecules. Although the significance of the observed R p /R s variations is low, if confirmed, this fact would suggest that GJ3470b does not have a thick cloud layer in the atmosphere. This property would offer a wealth of opportunity for future transmission-spectroscopic observations of this planet to search for certain molecular features, such as H 2 O, CH 4 , and CO, without being prevented by clouds. Subject headings: planetary systems -planets and satellites: atmosphere -planets and satellites:individual(GJ3470b) -stars: individual(GJ3470) -techniques: photometric

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Section: Mitsume Optical Observationsmentioning

confidence: 99%

OPTICAL-TO-NEAR-INFRARED SIMULTANEOUS OBSERVATIONS FOR THE HOT URANUS GJ3470b: A HINT OF A CLOUD-FREE ATMOSPHERE

Fukui¹,

Narita²,

Kurosaki³

et al. 2013

ApJ

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“…There were some operational issues encountered during the operation with ProdAgent [4]. Of which 100% accountability had the highest priority.…”

Section: Prodagent Vs Wmagentmentioning

confidence: 99%

A new era for central processing and production in CMS

Fajardo

Gutsche

Foulkes

et al. 2012

J. Phys.: Conf. Ser.

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The goal for CMS computing is to maximise the throughput of simulated event generation while also processing the real data events as quickly and reliably as possible. To maintain this achievement as the quantity of events increases, since the beginning of 2011 CMS computing has migrated at the Tier 1 level from its old production framework, ProdAgent, to a new one, WMAgent. The WMAgent framework offers improved processing efficiency and increased resource usage as well as a reduction in manpower. In addition to the challenges encountered during the design of the WMAgent framework, several operational issues have arisen during its commissioning. The largest operational challenges were in the usage and monitoring of resources, mainly a result of a change in the way work is allocated. Instead of work being assigned to operators, all work is centrally injected and managed in the Request Manager system and the task of the operators has changed from running individual workflows to monitoring the global workload. In this report we present how we tackled some of the operational challenges, and how we benefitted from the lessons learned in the commissioning of the WMAgent framework at the Tier 2 level in late 2011. As case studies, we will show how the WMAgent system performed during some of the large data reprocessing and Monte Carlo simulation campaigns.

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“…The SDSS includes two spectroscopic galaxy surveys: the main galaxy sample which is complete to a reddening-corrected Petrosian r magnitude brighter than 17.77, and a deeper sample of luminous red galaxy sample selected based on both colour and magnitude [18]. The SDSS has regular public data releases: the 4th data release in 2005 included 480000 independent galaxy spectra [1]. When completed, the SDSS will have obtained spectra for ∼ 10 6 galaxies.…”

Section: Brief Description Of Redshift Surveysmentioning

confidence: 99%

Cosmological Constraints from Galaxy Clustering

Percival

2007

Lecture Notes in Physics

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In this manuscript I review the mathematics and physics that underpins recent work using the clustering of galaxies to derive cosmological model constraints. I start by describing the basic concepts, and gradually move on to some of the complexities involved in analysing galaxy redshift surveys, focusing on the 2dF Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky survey (SDSS). Difficulties within such an analysis, particularly dealing with redshift space distortions and galaxy bias are highlighted. I then describe current observations of the CMB fluctuation power spectrum, and consider the importance of measurements of the clustering of galaxies in light of recent experiments. Finally, I provide an example joint analysis of the latest CMB and large-scale structure data, leading to a set of parameter constraints.

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CMS distributed computing workflow experience

Abstract: The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Adelman-McCarthy, Jennifer et al. "CMS distributed computing workflow experience.

Cited by 3 publications

References 4 publications

OPTICAL-TO-NEAR-INFRARED SIMULTANEOUS OBSERVATIONS FOR THE HOT URANUS GJ3470b: A HINT OF A CLOUD-FREE ATMOSPHERE

OPTICAL-TO-NEAR-INFRARED SIMULTANEOUS OBSERVATIONS FOR THE HOT URANUS GJ3470b: A HINT OF A CLOUD-FREE ATMOSPHERE

A new era for central processing and production in CMS

Cosmological Constraints from Galaxy Clustering

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