A code to Make Your Own Synthetic ObservaTIonS (MYOSOTIS). Issue 3 (17th February 2019)

• Record Type: Journal Article
• Authors: Khorrami, Zeinab; Khalaj, Pouria; Buckner, Anne S M; Clark, Paul C; Moraux, Estelle; Lumsden, Stuart; Joncour, Isabelle; Oudmaijer, René D; de la Calle, Ignacio; Herrera-Fernandez, José M; Motte, Frédérique; Blanco, José Manuel; Valero-Martin, Luis
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 485:Issue 3(2019)
• Page Start: 3124
• Page End: 3133
• Publication Date: 2019-02-17
• Subjects: instrumentation: adaptive optics -- instrumentation: high angular resolution -- techniques: photometric -- telescopes -- stars: luminosity function, mass function -- open clusters and associations: general; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz490
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We introduce our new code myosotis (Make Your Own Synthetic ObservaTIonS) which is designed to produce synthetic observations from simulated clusters. The code can synthesize observations from both ground- and spaced-based observatories, for a range of different filters, observational conditions and angular/spectral resolution. In this paper, we highlight some of the features of myosotis, creating synthetic observations from young massive star clusters. Our model clusters are simulated using nbody6 code and have different total masses, half-mass radii, and binary fractions. The synthetic observations are made at the age of 2 Myr with Solar metallicity and under different extinction conditions. For each cluster, we create synthetic images of the Hubble Space Telescope ( HST ) in the visible (WFPC2/ F 555 W ) as well as Very Large Telescopes in the nearIR (SPHERE/IRDIS/ K s ). We show how myosotis can be used to look at mass function (MF) determinations. For this aim we re-estimate stellar masses using a photometric analysis on the synthetic images. The synthetic MF slopes are compared to their actual values. Our photometric analysis demonstrate that depending on the adopted filter, extinction, angular resolution, and pixel sampling of the instruments, the power-law index of the underlying MFs can be shallower than the observed ones by at least ±0.25 dex which is in agreement with the observed discrepancies reported in the literature, specially for young star clusters.