Fermi Sample Clauses

Fermi. At least 30+ MSPs were found using such surveys over the past few years (Roberts 2011). The two original BWP systems show eclipses of the radio emission from the pulsar, which are thought to originate from the compan- ion star and be broadened by material being ablated off of the companion star by a strong pulsar wind (Fruchter et al. 1988; Stappers et al. 1996; Chen et al. 2013). The BWPs are, due to the ablated material, often complicated systems to use for precision timing. The companion stars are often bloated, and they exert small torques on the system, which will then cause small changes in the orbit. The changes in the orbit increase the number of parameters that is required in timing models, and their variability could reduce the sensitivity of the timing solution to the gravitational wave (GW) signals (Bochenek et al. 2015). By observing multiple stable pulsars in different parts of the sky, an array of pulsars, and cross-correlating the timing residuals from the different pulsars, it should be possible to obtain the sensitivity to measure the expected quadrapolar signature of a GW. This is the general idea behind the pulsar timing arrays (PTAs) (Lentati et al. 2015). With new BWPs being discovered, Bochenek et al. (2015) tested the feasibility of using BWPs in the pulsar timing arrays, by testing if fitting for multiple orbital frequency derivatives was significantly reducing the sensitivity to the GW signal. Bochenek et al. (2015) used simulated data sets of five different pulsars to constrain how sensitive to a GW signal a timing solution would be, if several orbital period derivatives were fitted for. They found that the sensitivity to the GW signals were − not reduced significantly, partly due to GW signals spanning several years and the typical BWP orbit spans 2 to 20 hr. It was thus concluded that some BWPs could be used in pulsar timing arrays, and PSR J0610 2100 is already used by the PTAs (Desvignes et al. 2016). There are three other BWPs that are stable and which are candidates for the PTAs: PSRs J0023+0923, J2214+3000 and J2234+0944. All three are currently observed by the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) (Arzoumanian et al. 2018) and the European Pulsar Timing Array (EPTA) (this work). PSR J0023+0923 was discovered with the Green Bank Telescope (GBT) through the survey of Fermi γ-ray sources (Hessels et al. 2011). PSR J0023+0923 is a mil- lisecond pulsar with a spin period of ∼3 ms, an orbital p...
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Fermi is entitled to assign, transfer, charge or otherwise deal with any of its rights or obligations under this Agreement to any of its Affiliates only with the prior written consent of BV Ozon LP, which cannot be unreasonably withheld, if (i) BV Ozon LP is satisfied with the Affiliate’s identity and creditworthiness, and (ii) the Affiliate enters into and executes such documents as may be reasonably requested by BV Ozon LP to ensure that BV Ozon LP’s position as set out in this Agreement and any related agreement(s) is not prejudiced.
Fermi is entitled to assign, transfer, charge or otherwise deal with any of its rights or obligations under this Agreement to any of its Affiliates only with the prior written consent of BVFVNL, which cannot be unreasonably withheld, if (i) BVFVNL is satisfied with the Affiliate’s identity and creditworthiness, and (ii) the Affiliate enters into and executes such documents as may be reasonably requested by BVFVNL to ensure that BVFVNL’s position as set out in this Agreement and any related agreement(s) is not prejudiced.

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