The next generation Virgo cluster survey (NGVS) I Introduction to the survey
Texto completo
Documento similar
These two models are then used to calculate the number of SLSNe-I, in bins of ∆z = 0.5 width, centred on multiples of z = 0.5 up to z = 3.5 which is consistent with the highest
MD simulations in this and previous work has allowed us to propose a relation between the nature of the interactions at the interface and the observed properties of nanofluids:
Government policy varies between nations and this guidance sets out the need for balanced decision-making about ways of working, and the ongoing safety considerations
Mart in point ed out t hat t he artificial upturn in the lower main sequence is a common artefact in global-fits and is caused by the breakdown of Fe ionization balance at low t
✴ WEAVE , IFU mode (fov = 2 sq. arcmin, with 1-2.5 arcsec/sparxel) to trace the stellar population of galaxies beyond 3 HLR in a large sample of galaxies covering all
The main scientific driver of the survey is to study the Initial Mass Function and its dependence with environment in the substellar regime using a uniformly selected data set
In the previous sections we have shown how astronomical alignments and solar hierophanies – with a common interest in the solstices − were substantiated in the
Relationship between the total cluster stellar mass and the photometric blue fraction for the ALHAMBRA cluster and group sample stacked into different redshift bins. The galaxy