-
Hi,
I am having the same error detailed in issue #9. In that case they mention that the filter curve was the problem, but I am using NIRCam filters taken directly from [SVO](http://svo2.cab.inta-cs…
-
Now that we have the Padova/Colibri models incorporated into the downloadable data #357 , we need some criteria for when to use the models for a given star. At the moment we are not assuming any dust …
-
The output mass on the prospector is the ever-formed stellar mass, right?
How can this be changed? so that the output is the surviving stellar mass? I think I should pass add_stellar_remnants = Fal…
-
As discussed in #17 and raised by @kstassun, "Flicker" noise is an excellent way to characterize stellar properties using photometric time series. Flicker noise occurs due to the granulation on the su…
-
The IDL Hammer version returned a table of equivalent widths and band measurements, especially Balmer series and TiO values (particularly useful for low-mass star work, and computing *zeta*). Any hope…
-
对于如下内容:
```python
Massive ($\gtrsim9$ M$_\odot$) and very massive ($\gtrsim100$ M$_\odot$) stars are expected to release large amounts of energy and metal-enriched material throughout their relative…
-
- I suggest moving the grouping of the 6 science themes to be before the list of the themes. I think this comes across clearer if you first create the bin of "Galaxy formation and evolution" and defi…
-
Now we have a forward model $f(\vec{\theta})$ (an NN emulator) which could return the SED of given physical parameters. Then we need to build a neural density estimator to describe the $P(\vec{\theta}…
-
**Describe the bug**
When running large populations, I occasionally (rarely, something like 1 in 10^5 binaries) get the following error:
ERROR: in Early_Asymptotic_Giant_Branch::double GiantBranc…
-
#### TLDR
After creating an isochrone object, changing the filters, while keep all else constant, does not cause SPISEA to not recalculate that isochrone.
#### Suspected cause
This appears to be…