ngvla The Next Generation Very Large Array

Transcription

1 NATIONAL RADIO ASTRONOMY OBSERVATORY From the VLA to the ngvla Luis F. Rodríguez Ins2tuto de Radioastronomía y Astro8sica, UNAM ngvla

2 Thinking in the next genera4on of instruments A source of ideas and challenges are the things that you cannot do with the present instruments. However, serendipity will probably produce the most exci2ng and unexpected results of the new instrument.

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5 Fast improvement in the field of disks The case of TW Hya D=54 pc Age=9 million years VLA: 7 mm SMA: 870 μm ALMA: 870 μm Wilner et al. (2000) Andrews et al. (2012) Andrews et al. (2016)

6 Disk fever: major topic in astronomical literature

7 HL ALMA; 1.3 mm! The most detailed and highest quality image of a circumstellar disk (Brogan et al. 2015)!

8 Emission at all ALMA wavelengths is optically thick Pinte et al. (2016)! Jin et al. (2016)!

9 ALMA emission is optically thick at the densest parts,! In particular the internal disk (<50 AU),! where terrestrial planets are expected to form.!

10 high sensitive, high angular resolution observations at 7 mm! >15 hr of observation at Q band with excellent atmospheric conditions! Carrasco-González Carrasco-González et al. (2016)! et al. (2017)!

11 Dust emission at 7 mm is optically thin!

12 1. Mass distribution in the disk! The most internal features of the disk are much more massive than previously inferred!

13 2. Grain Size Distribution! Large Small

14 3. Substructure Within the Rings! 1.3 mm! Carrasco-González et al. (2017)! 7 mm!

15 Problem at long wavelengths: The JET! Lumbreras et al., in prep.!

16 You need to understand both the disk and the jet Characteriza2on of free-free emission will require very sensi2ve, high angular resolu2on observa2ons at cen2meter wavelengths, not only a 7 mm. Disentangle dust emission from free-free emission. Also other freefree mechanisms such as photoevaporated disks could be present and excellent data will be needed to dis2nguish it from jets.

17 The case of the transi4on disk of UX Tau A D=138 pc ALMA 1.3 mm Colors: CO velocity Black contours: 1.3 mm con2nuum White contours: VLA 7 mm con2nuum Note smoothness at 1.3 mm versus clumpiness at 7 mm Zapata et al. (2017)

18 Comparing two op4cally-thin images: Rota4on?

19 HH 212: Indirect determina4on of jet launching radius ALMA data Orange = 352 GHz dust con2nuum Green, blue, violet = SiO J=8-7 transi2on Lee et al. (2017)

20 HH 212 (Lee et al. 2017) è r AU

21 The jet is also detected as faint, compact VLA source HH 212 VLA-A, X-band Jet detected at 40±10 μjy Galván-Madrid et al. (2004) ngvla will reach resolu2on of 1 AU in nearby regions of star forma2on, allowing the best direct es2mate of jet launching and collima2on scales.

22 Radio recombina4on lines from jets and other faint free-free sources (stellar winds, UCHII regions) Wide (100s of km/s), weak lines in the cen2meter regime. Assume jet or wind: S C (ν) goes as ν 0.6 Assume line has Δν = 300 km s -1 Anglada et al. (2017) Further assume S C (10 GHz) = 1 mjy è S L (10 GHz) = 8 μjy Which present-day VLA band gives you the best chance?

23 Radio recombina4on lines from protostellar jets Channels of 100 km s -1, 20 hours total 4me, stacking all lines in band. Band Frequency (GHz) Number of RRL Noise in channel (μjy) RRL flux density (μjy) L S C X Ku K Ka Q Signal-to-noise raeo

24 Many other important problems in Craddle of Life Requirements on: Sensi2vity Angular Resolu2on Spectroscopy Polariza2on Extended emission Variability in 2me Murphy et al. (2017)

25 Conclusions The study of disks and jets will require of observa2ons over a wide range of frequencies to obtain op2cally-thin emission images and to correct for contribu2on of free-free. Also need to understand different sources of free-free. The possibility of imaging radio recombina2on lines from free-free jets and very faint HII regions will be valuable for kinema2cs. The ngvla will be key instrument for these observa2ons and many other related to star forma2on.