Field guide section on YSOs

config.defaults.yaml

@@ -86,10 +86,46 @@ docs:
     flaring_mdwarf:
       coordinates: [103.289525, 10.194726]
       title: M dwarf (Flaring)
+    cv_U_Gem:
+      coordinates: [18.884181, 37.626534]
+      title: Cataclysmic variable (U Gem dwarf nova)
+    cv_Z_Cam:
+      coordinates: [269.093260, 2.967803]
+      title: Cataclysmic variable (Z Cam dwarf nova)
+    cv_SU_UMa:
+      coordinates: [170.883476, 43.288214]
+      title: Cataclysmic variable (SU UMa/WZ Sge dwarf nova)
+    cv_Novalike:
+      coordinates: [322.961689, 49.233813]
+      title: Cataclysmic variable (Novalike)
     mira:
       coordinates: [9.1523, 68.0221]
       period: 212.0066035
       title: A Mira (Long Period Variable)
     srv:
       coordinates: [330.302266, 66.153712]
       title: Semi Regular Variable
+    yso_sinusoidal:
+      coordinates: [313.30835,44.21604]
+      title: YSO Sinusoidal
+    yso_quasi-periodic:
+      coordinates: [313.42558,44.44825]
+      title: YSO quasi-periodic
+    yso_stochastic:
+      coordinates: [313.364708,44.10261]
+      title: YSO stochastic
+    yso_burster:
+      coordinates: [313.31515,43.73967]
+      title: YSO burster
+    yso_outburster:
+      coordinates: [301.2751339,  36.4870689]
+      title: YSO outburster
+    yso_dipper:
+      coordinates: [313.417297,44.17929]
+      title: YSO dipper
+    yso_fader:
+      coordinates: [312.85172,44.217837]
+      title: YSO fader
+    yso_longterm-drifter:
+      coordinates: [314.57094,43.89535]
+      title: YSO longterm-drifter

data/golden/yso.csv

@@ -0,0 +1,101 @@
+ra,dec
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doc/field_guide.md

@@ -29,3 +29,6 @@ for more details on the taxonomy.
 
 ```{include} ./field_guide__lpv.md
 ```
+
+```{include} ./field_guide__yso.md
+```

doc/field_guide__yso.md

@@ -0,0 +1,76 @@
+## Young Stellar Objects (yso)
+
+Young stellar objects (YSOs) exhibit a wide range of variability types,
+with many subclasses depending on the dominant physics in the system.
+
+
+Some of the lightcurve possibilities for YSOs include:
+
+
+
+
+### Classification and numbers
+- Supertypes
+  - Variable
+- Subtypes
+  - simple sinusoidal
+  - quasi-periodic
+  - stochastic
+  - faders
+  - longterm drifters
+- Occurrence rate: common, about 10<sup>X</sup> expected in ZTF data
+
+
+### ZTF light curves
+![ZTF yso sinusoidal](data/yso_sinusoidal.png)
+![ZTF yso quasi-periodic](data/yso_quasi-periodic.png)
+![ZTF yso stochastic](data/yso_stochastic.png)
+![ZTF yso burster](data/yso_burster.png)
+![ZTF yso outburster](data/yso_outburster.png)
+![ZTF yso dipper](data/yso_dipper.png)
+![ZTF yso fader](data/yso_fader.png)
+![ZTF yso longterm-drifter](data/yso_longterm-drifter.png)
+
+#### Description
+YSOs are not smooth variables like pulsating (e.g. RR Lyr) or eclipsing (e.g. Algol or EA) classes.
+Instead, because the lightcurves are generally the result of several superposed physical effects,
+they can appear quite messy,  They thus may satisfy the criteria for two or even more of the lightcurve categories below.
+Yet one subclass often dominates.
+
+#### Light curve characteristics
+- simple sinusoidal periodicity
+ (caused by rotating star with cool or hot spots)
+
+- quasi-periodic behavior, which is a periodicity on which stochastic behavior is superposed
+(caused by accreting star with rotational modulation)
+
+- stochastics, appearing similar to a damped random walk, with time scales from hours to weeks and usually symmetric around a mean (caused by accreting star with accretion effects dominating rotation effects)
+
+- bursts, which are brightening episodes that can last from many hours to days or possibly weeks; they are longer than flares which decay within minutes to hours
+(caused by clumpy accretion, rather than smooth accretion, due to a build-up of material in the transition zone between the stellar magnetosphere and the disk);
+
+- outbursts, like the above, but much larger amplitudes of 2-5 mag and much longer durations of months to decades
+(caused by accretion events driven by instabilities in the magnetosphere/disk interaction region, or the inner disk);
+
+- dippers, which have timescales similar to bursts, but are fading events of a few percent to tens of percent, rather than brightening, and can last many hours to days
+(caused by dust in the magnetosphere/disk interaction region that can be co-rotating with the star, in which case the source could be called a quasi-periodic dipper);
+
+- faders, like the above, but much larger amplitudes of 2-5 mag and longer durations, of weeks to years
+(caused by dust that is somewhat further out in the disk and has rotated into the line of sight).
+
+- longterm drifting behavior over a significant fraction of the time series, with gradual dimming or brightening over months to years
+(caused by slowly evolving changes in extinction or accretion)
+
+#### Other characteristics and selection methods
+ - In addition to the variability characteristics described above, young stellar objects must reside
+above the main sequence, as they are still contracting and are not yet
+stable hydrogen burning objects on the main sequence.   The periodic objects
+typically lack disks, but the other variability classes typically have
+infrared excess (large WISE or 2MASS colors) that imply the presence of a disk.
+
+![HR diagram of YSO](data/hr__yso.png)
+
+![RA/Dec diagram of YSO](data/radec__yso.png)
+
+### References and further reading:
+-